[ { "id": "authors:hjsz2-f4a98", "collection": "authors", "collection_id": "hjsz2-f4a98", "cite_using_url": "https://authors.library.caltech.edu/records/hjsz2-f4a98", "type": "article", "title": "Rise of the Forsaken Relics: Connecting Present-day Stellar Streams and Phase-mixed Galaxies to the Epoch of Reionization", "author": [ { "family_name": "Kundu", "given_name": "Aritra", "orcid": "0000-0001-8746-4753" }, { "family_name": "Sanderson", "given_name": "Robyn", "orcid": "0000-0003-3939-3297" }, { "family_name": "Lidz", "given_name": "Adam", "orcid": "0000-0002-3950-9598" }, { "family_name": "Gandhi", "given_name": "Pratik J.", "orcid": "0000-0003-0965-605X" }, { "family_name": "Wetzel", "given_name": "Andrew", "orcid": "0000-0003-0603-8942" }, { "family_name": "Feldmann", "given_name": "Robert", "orcid": "0000-0002-1109-1919" }, { "family_name": "Panithanpaisal", "given_name": "Nondh", "orcid": "0000-0001-5214-8822", "clpid": "Panithanpaisal-Nondh" }, { "family_name": "Singh", "given_name": "Jasjeev", "orcid": "0009-0008-8901-2206" }, { "family_name": "Boylan-Kolchin", "given_name": "Michael", "orcid": "0000-0002-9604-343X" } ], "abstract": "
\n

The “near–far” approach to studying reionization leverages the star formation histories of the Milky Way (MW) or Local Group (LG) galaxies, derived from resolved photometry, to infer the low-mass/faint end of the stellar mass functions (SMFs) or the ultraviolet luminosity functions (UVLFs) of high-redshift galaxies (z \u2273 6), beyond the current James Webb Space Telescope detection limits (MUV \u2273 −15). Previous works considered only intact low-mass galaxies in the MW and LG, neglecting disrupted galaxies such as stellar streams and phase-mixed objects. Using the FIRE-2 simulations, we show that these disrupted galaxies contribute up to ∼50% of the total stellar-mass budget of the proto-MW/LG at z = 6−9. Including all the progenitors of these disrupted galaxies improves the normalization of the recovered SMFs/UVLFs by factors of ∼2–3 and reduces the halo-to-halo variation in the slope by ∼20%–40%. This enables robust constraints down to at least the resolution limit of the simulations, near M\u22c6 ∼ 105M\u2299or MUV ∼ −10 at z \u2273 6. We also show that “fossil-record” reconstructions—which assume each present-day system descends from a single reionization-era progenitor—are sensitive to the stellar-mass/UV-magnitude thresholds, which introduces bias in the inferred slopes at the low-mass/faint end. Additionally, we demonstrate that neglecting disrupted systems underestimates the contribution of galaxies with MUV \u2272 −15 to the reionization-era UV luminosity density. Finally, we estimate that a significant fraction (∼50%) of streams with M\u22c6 \u2273 106M\u2299 at z = 0 should be detectable from upcoming Rubin Observatory and Roman Space Telescope observations.

\n
", "doi": "10.3847/1538-4357/ae32eb", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2026-03-01", "series_number": "1", "volume": "999", "issue": "1", "pages": "124" }, { "id": "authors:ys67b-7ws70", "collection": "authors", "collection_id": "ys67b-7ws70", "cite_using_url": "https://authors.library.caltech.edu/records/ys67b-7ws70", "type": "article", "title": "Breaking Down the CosmoGEMS: Toward Modeling and Understanding Globular Cluster Stellar Streams in a Fully Cosmological Context", "author": [ { "family_name": "Panithanpaisal", "given_name": "Nondh", "orcid": "0000-0001-5214-8822", "clpid": "Panithanpaisal-Nondh" }, { "family_name": "Sanderson", "given_name": "Robyn E.", "orcid": "0000-0003-3939-3297" }, { "family_name": "Rodriguez", "given_name": "Carl L.", "orcid": "0000-0003-4175-8881" }, { "family_name": "Starkenburg", "given_name": "Tjitske", "orcid": "0000-0003-2539-8206" }, { "family_name": "Pearson", "given_name": "Sarah", "orcid": "0000-0003-0256-5446" }, { "family_name": "Bonaca", "given_name": "Ana", "orcid": "0000-0002-7846-9787" }, { "family_name": "Hopkins", "given_name": "Philip F.", "orcid": "0000-0003-3729-1684", "clpid": "Hopkins-P-F" }, { "family_name": "Cook", "given_name": "Brian T.", "orcid": "0000-0003-0341-6928" }, { "family_name": "Arora", "given_name": "Arpit", "orcid": "0000-0002-8354-7356" }, { "family_name": "Weatherford", "given_name": "Newlin C.", "orcid": "0000-0002-9660-9085" } ], "abstract": "

Next-generation surveys are expected to uncover thousands of globular cluster (GC) stellar streams, motivating the need for a theoretical framework that produces realistic GC streams in a fully cosmological, Milky Way–like environment. We present CosmoGEMS , a star-by-star cosmological GC stream framework that self-consistently links small-scale cluster physics with large-scale Galactic dynamics. The initial phase-space positions of stream stars are informed by post-processed GC populations within the FIRE cosmological simulation. Escaped stars are orbit-integrated from their time of escape to the present day in a time-evolving Galactic potential extracted from the same simulation using a basis function expansion. We explore two example streams on different orbits. One forms a long, thin stream with a velocity dispersion consistent with Milky Way GC streams. However, it exhibits a clump and orbital-phase-dependent misalignments due to the evolving potential. The other stream develops both a thin component and a diffuse, shell-like structure, similar to features observed in streams like Jhelum. These results highlight the power of fully cosmological models in producing realistic stream morphologies and kinematics. Unlike idealized simulations, our models naturally incorporate time-dependent changes in the progenitor's orbit, including orbital plane evolution, which significantly affects stream structure. This challenges common assumptions in stream-finding algorithms and interpretation. CosmoGEMS provides a key step toward connecting future stellar stream observations with the physics of GC evolution and hierarchical galaxy formation in a cosmological context.

", "doi": "10.3847/1538-4357/ae2ea7", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2026-02-01", "series_number": "2", "volume": "997", "issue": "2", "pages": "182" }, { "id": "authors:kq6bz-gdy07", "collection": "authors", "collection_id": "kq6bz-gdy07", "cite_using_url": "https://authors.library.caltech.edu/records/kq6bz-gdy07", "type": "article", "title": "Cosmological Predictions for Minor Axis Stellar Density Profiles in the Inner Regions of Milky Way\u2013mass Galaxies", "author": [ { "family_name": "Lucey", "given_name": "Madeline", "orcid": "0000-0001-7297-8508" }, { "family_name": "Sanderson", "given_name": "Robyn E.", "orcid": "0000-0003-3939-3297" }, { "family_name": "Horta", "given_name": "Danny", "orcid": "0000-0003-1856-2151" }, { "family_name": "Kundu", "given_name": "Aritra", "orcid": "0000-0001-8746-4753" }, { "family_name": "Hopkins", "given_name": "Philip F.", "orcid": "0000-0003-3729-1684", "clpid": "Hopkins-P-F" }, { "family_name": "Arora", "given_name": "Arpit", "orcid": "0000-0002-8354-7356" }, { "family_name": "Singh", "given_name": "Jasjeev", "orcid": "0009-0008-8901-2206" }, { "family_name": "Panithanpaisal", "given_name": "Nondh", "orcid": "0000-0001-5214-8822", "clpid": "Panithanpaisal-Nondh" } ], "abstract": "
\n

ΛCDM cosmology predicts the hierarchical formation of galaxies, which build up mass by merger events and accreting smaller systems. The stellar halo of the Milky Way (MW) has proven to be useful a tool for tracing this accretion history. However, most of this work has focused on the outer halo where dynamical times are large and the dynamical properties of accreted systems are preserved. In this work, we investigate the inner galaxy regime, where dynamical times are relatively small and systems are generally completely phase mixed. Using the FIRE-2 and Auriga cosmological zoom-in simulation suites of MW-mass galaxies, we find the stellar density profiles along the minor axis (perpendicular to the galactic disk) within the Navarro–Frenk–White scale radii (R ≈ 15 kpc) are best described as an exponential disk with scale height < 0.3 kpc and a power-law component with slope α ≈ −4. The stellar density amplitude and slope for the power-law component are not significantly correlated with metrics of the galaxy's accretion history. Instead, we find the stellar profiles strongly correlate with the dark matter profile. Across simulation suites, the galaxies studied in this work have a stellar-to-dark-matter mass ratio that decreases as 1/r2 along the minor axis.

\n
", "doi": "10.3847/1538-4357/adb9e8", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2025-04-01", "series_number": "2", "volume": "982", "issue": "2", "pages": "87" }, { "id": "authors:91ke9-z1r13", "collection": "authors", "collection_id": "91ke9-z1r13", "cite_using_url": "https://authors.library.caltech.edu/records/91ke9-z1r13", "type": "article", "title": "Efficient and Accurate Force Replay in Cosmological-baryonic Simulations", "author": [ { "family_name": "Arora", "given_name": "Arpit", "orcid": "0000-0002-8354-7356" }, { "family_name": "Sanderson", "given_name": "Robyn", "orcid": "0000-0003-3939-3297" }, { "family_name": "Regan", "given_name": "Christopher" }, { "family_name": "Garavito-Camargo", "given_name": "Nicol\u00e1s", "orcid": "0000-0001-7107-1744" }, { "family_name": "Bregou", "given_name": "Emily", "orcid": "0000-0003-3792-8665" }, { "family_name": "Panithanpaisal", "given_name": "Nondh", "orcid": "0000-0001-5214-8822", "clpid": "Panithanpaisal-Nondh" }, { "family_name": "Wetzel", "given_name": "Andrew", "orcid": "0000-0003-0603-8942" }, { "family_name": "Cunningham", "given_name": "Emily C.", "orcid": "0000-0002-6993-0826" }, { "family_name": "Loebman", "given_name": "Sarah R.", "orcid": "0000-0003-3217-5967" }, { "family_name": "Dropulic", "given_name": "Adriana", "orcid": "0000-0002-7352-6252" }, { "family_name": "Shipp", "given_name": "Nora", "orcid": "0000-0003-2497-091X" } ], "abstract": "

We construct time-evolving gravitational potential models for a Milky Way–mass galaxy from the FIRE-2 suite of cosmological-baryonic simulations using basis function expansions. These models capture the angular variation with spherical harmonics for the halo and azimuthal harmonics for the disk, and the radial or meridional plane variation with splines. We fit low-order expansions (four angular/harmonic terms) to the galaxy's potential for each snapshot, spaced roughly 25 Myr apart, over the last 4 Gyr of its evolution, then extract the forces at discrete times and interpolate them between adjacent snapshots for forward orbit integration. Our method reconstructs the forces felt by simulation particles with high fidelity, with 95% of both stars and dark matter, outside of self-gravitating subhalos, exhibiting errors ≤4% in both the disk and the halo. Imposing symmetry on the model systematically increases these errors, particularly for disk particles, which show greater sensitivity to imposed symmetries. The majority of orbits recovered using the models exhibit positional errors ≤10% for 2–3 orbital periods, with higher errors for orbits that spend more time near the galactic center. Approximate integrals of motion are retrieved with high accuracy even with a larger potential sampling interval of 200 Myr. After 4 Gyr of integration, 43% and 70% of orbits have total energy and angular momentum errors within 10%, respectively. Consequently, there is higher reliability in orbital shape parameters such as pericenters and apocenters, with errors ∼10% even after multiple orbital periods. These techniques have diverse applications, including studying satellite disruption in cosmological contexts.

", "doi": "10.3847/1538-4357/ad88f0", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2024-12-10", "series_number": "1", "volume": "977", "issue": "1", "pages": "23" }, { "id": "authors:acfch-psa52", "collection": "authors", "collection_id": "acfch-psa52", "cite_using_url": "https://authors.library.caltech.edu/records/acfch-psa52", "type": "article", "title": "Public Data Release of the FIRE-2 Cosmological Zoom-in Simulations of Galaxy Formation", "author": [ { "family_name": "Wetzel", "given_name": "Andrew", "orcid": "0000-0003-0603-8942", "clpid": "Wetzel-Andrew-R" }, { "family_name": "Hayward", "given_name": "Christopher C.", "orcid": "0000-0003-4073-3236", "clpid": "Hayward-Christopher-C" }, { "family_name": "Sanderson", "given_name": "Robyn E.", "orcid": "0000-0003-3939-3297", "clpid": "Sanderson-Robyn-E" }, { "family_name": "Ma", "given_name": "Xiangcheng", "orcid": "0000-0001-8091-2349", "clpid": "Ma-Xiangcheng" }, { "family_name": "Angl\u00e9s-Alc\u00e1zar", "given_name": "Daniel", "orcid": "0000-0001-5769-4945", "clpid": "Angl\u00e9s-Alc\u00e1zar-Daniel" }, { "family_name": "Feldmann", "given_name": "Robert", "orcid": "0000-0002-1109-1919", "clpid": "Feldmann-Robert" }, { "family_name": "Chan", "given_name": "T. K.", "orcid": "0000-0003-2544-054X", "clpid": "Chan-Tsang-Keung" }, { "family_name": "El-Badry", "given_name": "Kareem", "orcid": "0000-0002-6871-1752", "clpid": "El-Badry-Kareem" }, { "family_name": "Wheeler", "given_name": "Coral", "clpid": "Wheeler-Coral-R" }, { "family_name": "Garrison-Kimmel", "given_name": "Shea", "orcid": "0000-0002-4655-8128", "clpid": "Garrison-Kimmel-Shea" }, { "family_name": "Nikakhtar", "given_name": "Farnik", "orcid": "0000-0002-3641-4366", "clpid": "Nikakhtar-Farnik" }, { "family_name": "Panithanpaisal", "given_name": "Nondh", "orcid": "0000-0001-5214-8822", "clpid": "Panithanpaisal-Nondh" }, { "family_name": "Arora", "given_name": "Arpit", "orcid": "0000-0002-8354-7356", "clpid": "Arora-Arpit" }, { "family_name": "Gurvich", "given_name": "Alexander B.", "orcid": "0000-0002-6145-3674", "clpid": "Gurvich-Alexander-B" }, { "family_name": "Samuel", "given_name": "Jenna", "orcid": "0000-0002-8429-4100", "clpid": "Samuel-Jenna" }, { "family_name": "Sameie", "given_name": "Omid", "orcid": "0000-0003-4394-6085", "clpid": "Sameie-Omid" }, { "family_name": "Pandya", "given_name": "Viraj", "orcid": "0000-0002-2499-9205", "clpid": "Pandya-Viraj" }, { "family_name": "Hafen", "given_name": "Zachary", "orcid": "0000-0001-7326-1736", "clpid": "Hafen-Zachary-H" }, { "family_name": "Hummels", "given_name": "Cameron", "orcid": "0000-0002-3817-8133", "clpid": "Hummels-Cameron-B" }, { "family_name": "Loebman", "given_name": "Sarah", "orcid": "0000-0003-3217-5967", "clpid": "Loebman-Sarah-R" }, { "family_name": "Boylan-Kolchin", "given_name": "Michael", "orcid": "0000-0002-9604-343X", "clpid": "Boylan-Kolchin-Michael" }, { "family_name": "Bullock", "given_name": "James S.", "orcid": "0000-0003-4298-5082", "clpid": "Bullock-James-S" }, { "family_name": "Faucher-Gigu\u00e8re", "given_name": "Claude-Andr\u00e9", "orcid": "0000-0002-4900-6628", "clpid": "Faucher-Gigu\u00e8re-Claude-Andr\u00e9" }, { "family_name": "Kere\u0161", "given_name": "Du\u0161an", "orcid": "0000-0002-1666-7067", "clpid": "Kere\u0161-Du\u0161an" }, { "family_name": "Quataert", "given_name": "Eliot", "orcid": "0000-0001-9185-5044", "clpid": "Quataert-Eliot" }, { "family_name": "Hopkins", "given_name": "Philip F.", "orcid": "0000-0003-3729-1684", "clpid": "Hopkins-P-F" } ], "abstract": "
\n

We describe a public data release of the FIRE-2 cosmological zoom-in simulations of galaxy formation (available at http://flathub.flatironinstitute.org/fire) from the Feedback In Realistic Environments (FIRE) project. FIRE-2 simulations achieve parsec-scale resolution to explicitly model the multiphase interstellar medium while implementing direct models for stellar evolution and feedback, including stellar winds, core-collapse and Type Ia supernovae, radiation pressure, photoionization, and photoelectric heating. We release complete snapshots from three suites of simulations. The first comprises 20 simulations that zoom in on 14 Milky Way (MW)–mass galaxies, five SMC/LMC-mass galaxies, and four lower-mass galaxies including one ultrafaint; we release 39 snapshots across z = 0–10. The second comprises four massive galaxies, with 19 snapshots across z = 1–10. Finally, a high-redshift suite comprises 22 simulations, with 11 snapshots across z = 5–10. Each simulation also includes dozens of resolved lower-mass (satellite) galaxies in its zoom-in region. Snapshots include all stored properties for all dark matter, gas, and star particles, including 11 elemental abundances for stars and gas, and formation times (ages) of star particles. We also release accompanying (sub)halo catalogs, which include galaxy properties and member star particles. For the simulations to z = 0, including all MW-mass galaxies, we release the formation coordinates and an “ex situ” flag for all star particles, pointers to track particles across snapshots, catalogs of stellar streams, and multipole basis expansions for the halo mass distributions. We describe publicly available python packages for reading and analyzing these simulations.

\n
", "doi": "10.3847/1538-4365/acb99a", "issn": "0067-0049", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Supplement Series", "publication_date": "2023-04", "series_number": "2", "volume": "265", "issue": "2", "pages": "44" }, { "id": "authors:4s7vw-ytp34", "collection": "authors", "collection_id": "4s7vw-ytp34", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220805-757926000", "type": "article", "title": "Reading the CARDs: The Imprint of Accretion History in the Chemical Abundances of the Milky Way's Stellar Halo", "author": [ { "family_name": "Cunningham", "given_name": "Emily C.", "orcid": "0000-0002-6993-0826", "clpid": "Cunningham-Emily-C" }, { "family_name": "Sanderson", "given_name": "Robyn E.", "orcid": "0000-0003-3939-3297", "clpid": "Sanderson-Robyn-E" }, { "family_name": "Johnston", "given_name": "Kathryn V.", "orcid": "0000-0001-6244-6727", "clpid": "Johnston-Kathryn-V" }, { "family_name": "Panithanpaisal", "given_name": "Nondh", "orcid": "0000-0001-5214-8822", "clpid": "Panithanpaisal-Nondh" }, { "family_name": "Ness", "given_name": "Melissa K.", "orcid": "0000-0001-5082-6693", "clpid": "Ness-Melissa-K" }, { "family_name": "Wetzel", "given_name": "Andrew", "orcid": "0000-0003-0603-8942", "clpid": "Wetzel-Andrew-R" }, { "family_name": "Loebman", "given_name": "Sarah R.", "orcid": "0000-0003-3217-5967", "clpid": "Loebman-Sarah-R" }, { "family_name": "Escala", "given_name": "Ivanna", "orcid": "0000-0002-9933-9551", "clpid": "Escala-Ivanna" }, { "family_name": "Horta", "given_name": "Danny", "orcid": "0000-0003-1856-2151", "clpid": "Horta-Danny" }, { "family_name": "Faucher-Gigu\u00e8re", "given_name": "Claude-Andr\u00e9", "orcid": "0000-0002-4900-6628", "clpid": "Faucher-Gigu\u00e8re-Claude-Andr\u00e9" } ], "abstract": "In the era of large-scale spectroscopic surveys in the Local Group, we can explore using chemical abundances of halo stars to study the star formation and chemical enrichment histories of the dwarf galaxy progenitors of the Milky Way (MW) and M31 stellar halos. In this paper, we investigate using the chemical abundance ratio distributions (CARDs) of seven stellar halos from the Latte suite of FIRE-2 simulations. We attempt to infer galaxies' assembly histories by modeling the CARDs of the stellar halos of the Latte galaxies as a linear combination of template CARDs from disrupted dwarfs, with different stellar masses M_\u22c6 and quenching times t\u2081\u2080\u2080. We present a method for constructing these templates using present-day dwarf galaxies. For four of the seven Latte halos studied in this work, we recover the mass spectrum of accreted dwarfs to a precision of t\u2081\u2080\u2080, we find the residuals of 20%\u201330% for five of the seven simulations. We discuss the failure modes of this method, which arise from the diversity of star formation and chemical enrichment histories that dwarf galaxies can take. These failure cases can be robustly identified by the high model residuals. Although the CARDs modeling method does not successfully infer the assembly histories in these cases, the CARDs of these disrupted dwarfs contain signatures of their unusual formation histories. Our results are promising for using CARDs to learn more about the histories of the progenitors of the MW and M31 stellar halos.", "doi": "10.3847/1538-4357/ac78ea", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2022-08-01", "series_number": "2", "volume": "934", "issue": "2", "pages": "Art. No. 172" }, { "id": "authors:660ae-gaq52", "collection": "authors", "collection_id": "660ae-gaq52", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220816-222049142", "type": "monograph", "title": "Public data release of the FIRE-2 cosmological zoom-in simulations of galaxy formation", "author": [ { "family_name": "Wetzel", "given_name": "Andrew", "orcid": "0000-0003-0603-8942", "clpid": "Wetzel-Andrew-R" }, { "family_name": "Hayward", "given_name": "Christopher C.", "orcid": "0000-0003-4073-3236", "clpid": "Hayward-Christopher-C" }, { "family_name": "Sanderson", "given_name": "Robyn E.", "orcid": "0000-0003-3939-3297", "clpid": "Sanderson-Robyn-E" }, { "family_name": "Ma", "given_name": "Xiangcheng", "orcid": "0000-0001-8091-2349", "clpid": "Ma-Xiangcheng" }, { "family_name": "Angl\u00e9s-Alc\u00e1zar", "given_name": "Daniel", "orcid": "0000-0001-5769-4945", "clpid": "Angl\u00e9s-Alc\u00e1zar-Daniel" }, { "family_name": "Feldmann", "given_name": "Robert", "orcid": "0000-0002-1109-1919", "clpid": "Feldmann-Robert" }, { "family_name": "Chan", "given_name": "T. K.", "orcid": "0000-0003-2544-054X", "clpid": "Chan-Tsang-Keung" }, { "family_name": "El-Badry", "given_name": "Kareem", "orcid": "0000-0002-6871-1752", "clpid": "El-Badry-Kareem" }, { "family_name": "Wheeler", "given_name": "Coral", "clpid": "Wheeler-Coral-R" }, { "family_name": "Garrison-Kimmel", "given_name": "Shea", "orcid": "0000-0002-4655-8128", "clpid": "Garrison-Kimmel-Shea" }, { "family_name": "Nikakhtar", "given_name": "Farnik", "orcid": "0000-0002-3641-4366", "clpid": "Nikakhtar-Farnik" }, { "family_name": "Panithanpaisal", "given_name": "Nondh", "orcid": "0000-0001-5214-8822", "clpid": "Panithanpaisal-Nondh" }, { "family_name": "Arora", "given_name": "Arpit", "orcid": "0000-0002-8354-7356", "clpid": "Arora-Arpit" }, { "family_name": "Gurvich", "given_name": "Alexander B.", "orcid": "0000-0002-6145-3674", "clpid": "Gurvich-Alexander-B" }, { "family_name": "Samuel", "given_name": "Jenna", "orcid": "0000-0002-8429-4100", "clpid": "Samuel-Jenna" }, { "family_name": "Sameie", "given_name": "Omid", "orcid": "0000-0003-4394-6085", "clpid": "Sameie-Omid" }, { "family_name": "Pandya", "given_name": "Viraj", "orcid": "0000-0002-2499-9205", "clpid": "Pandya-Viraj" }, { "family_name": "Hafen", "given_name": "Zachary", "orcid": "0000-0001-7326-1736", "clpid": "Hafen-Zachary-H" }, { "family_name": "Hummels", "given_name": "Cameron", "orcid": "0000-0002-3817-8133", "clpid": "Hummels-Cameron-B" }, { "family_name": "Loebman", "given_name": "Sarah", "orcid": "0000-0003-3217-5967", "clpid": "Loebman-Sarah-R" }, { "family_name": "Boylan-Kolchin", "given_name": "Michael", "orcid": "0000-0002-9604-343X", "clpid": "Boylan-Kolchin-Michael" }, { "family_name": "Bullock", "given_name": "James S.", "orcid": "0000-0003-4298-5082", "clpid": "Bullock-James-S" }, { "family_name": "Faucher-Gigu\u00e8re", "given_name": "Claude-Andr\u00e9", "orcid": "0000-0002-4900-6628", "clpid": "Faucher-Gigu\u00e8re-Claude-Andr\u00e9" }, { "family_name": "Kere\u0161", "given_name": "Du\u0161an", "orcid": "0000-0002-1666-7067", "clpid": "Kere\u0161-Du\u0161an" }, { "family_name": "Quataert", "given_name": "Eliot", "orcid": "0000-0001-9185-5044", "clpid": "Quataert-Eliot" }, { "family_name": "Hopkins", "given_name": "Philip F.", "orcid": "0000-0003-3729-1684", "clpid": "Hopkins-P-F" } ], "abstract": "We describe a public data release of the FIRE-2 cosmological zoom-in simulations of galaxy formation, available at this http URL, from the Feedback In Realistic Environments (FIRE) project. The FIRE-2 simulations achieve parsec-scale resolution to explicitly model the multi-phase interstellar medium while implementing direct models for stellar evolution and feedback, including stellar winds, core-collapse and Ia supernovae, radiation pressure, photoionization, and photoelectric heating. We release complete snapshots from 3 suites of simulations. The first comprises 20 simulations that zoom in on 14 Milky Way-mass galaxies, 5 SMC/LMC-mass galaxies, and 4 lower-mass galaxies including 1 ultra-faint; we release snapshots at z = 0, 1, 2, 3, 4. The second comprises 4 more massive galaxies simulated to z = 1, with snapshots at z = 1, 2, 3, 4, 5, 6. Finally, a high-redshift suite comprises 22 simulations at z = 5 and 6. Each simulation also includes dozens of resolved lower-mass (satellite) galaxies in its zoom-in region. Snapshots include all stored properties for all dark matter, gas, and star particles, including 11 elemental abundances for stars and gas, and formation times (ages) of star particles. We also release accompanying (sub)halo catalogs, which include galaxy properties and member star particles. For the simulations to z = 0, including all Milky Way-mass galaxies, we release an \"ex-situ\" flag for star particles, pointers to track particles across snapshots, catalogs of stellar streams, and multipole basis expansions for the halo mass distributions. We describe several publicly available python packages for reading and analyzing these simulations.", "doi": "10.48550/arXiv.2202.06969", "publisher": "arXiv", "publication_date": "2022-02-14" } ]