Public data release of the FIRE-2 cosmological zoom-in simulations of galaxy formation

Creators: Wetzel, Andrew; Hayward, Christopher C.; Sanderson, Robyn E.; Ma, Xiangcheng; Anglés-Alcázar, Daniel; Feldmann, Robert; Chan, T. K.; El-Badry, Kareem; Wheeler, Coral; Garrison-Kimmel, Shea; Nikakhtar, Farnik; Panithanpaisal, Nondh; Arora, Arpit; Gurvich, Alexander B.; Samuel, Jenna; Sameie, Omid; Pandya, Viraj; Hafen, Zachary; Hummels, Cameron; Loebman, Sarah; Boylan-Kolchin, Michael; Bullock, James S.; Faucher-Giguère, Claude-André; Kereš, Dušan; Quataert, Eliot; Hopkins, Philip 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.

Additional Information

Attribution 4.0 International (CC BY 4.0). We generated the FIRE-2 simulations using: Stampede and Stampede 2, via the Extreme Science and Engineering Discovery Environment (XSEDE), supported by NSF grant ACI-1548562, including allocations TG-AST120025, TG-AST140023, TG-AST140064, TG-AST160048; Blue Waters, supported by the NSF; Frontera, supported by the NSF and TACC, including allocations AST21010 and AST20016; Pleiades, via the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center, including allocations HEC SMD-16-7592, SMD-16-7561, SMD-17-120; and the Quest computing cluster at Northwestern University. This work uses data hosted by the Flatiron Institute's FIRE data hub, and we generated data using the Flatiron Institute's computing clusters rusty and popeye; the Flatiron Institute is supported by the Simons Foundation. yt Hub is supported in part by the Gordon and Betty Moore Foundation's Data-Driven Discovery Initiative through Grant GBMF4561 to Matthew Turk and the National Science Foundation under Grant ACI-1535651. AW received support from: NSF CAREER award AST-2045928 and NSF grant AST-2107772; NASA ATP grants 80NSSC18K1097 and 80NSSC20K0513; HST grants GO-14734, AR-15057, AR-15809, GO-15902 from STScI; a Scialog Award from the Heising-Simons Foundation; and a Hellman Fellowship. RES and NP acknowledge support from NASA grant 19-ATP19-0068; and RES, FN, and AA acknowledge support from the Research Corporation through the Scialog Fellows program on Time Domain Astronomy, and from NSF grant AST-2007232; RES additionally acknowledges support from HST-AR-15809 from STScI. DAA was supported in part by NSF grants AST-2009687 and AST-2108944. TKC is supported by the Science and Technology Facilities Council (STFC) astronomy consolidated grant ST/P000541/1 and ST/T000244/1. JS was supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2102729. ZH was supported by a Gary A. McCue postdoctoral fellowship at UC Irvine. SL was supported by NSF grant AST-2109234 and HST-AR-16624 from STScI. MBK acknowledges support from NSF CAREER award AST-1752913, NSF grants AST-1910346 and AST-2108962, NASA grant NNX17AG29G, and HST grants AR-15006, AR-15809, GO-15658, GO-15901, GO-15902, AR-16159, GO-16226 from STScI. CAFG was supported by NSF through grants AST-1715216, AST-2108230, and CAREER award AST-1652522; by NASA through grants 17-ATP17-0067 and 21-ATP21-0036; by STScI through grant HST-AR-16124.001-A; and by the Research Corporation for Science Advancement through a Cottrell Scholar Award and a Scialog Award. DK was supported by NSF grants AST-1715101 and AST-2108314. Support for PFH was provided by NSF Research Grants 1911233, 20009234, 2108318, NSF CAREER grant 1455342, NASA grants 80NSSC18K0562, HST-AR-15800.

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