Статья

FIRE-2 simulations: physics versus numerics in galaxy formation

Philip F. HopkinsTAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USAAndrew WetzelCarnegie Observatories, Pasadena, CA 91101, USADušan KerešDepartment of Physics, Center for Astrophysics and Space Science, University of California at San Diego, 9500 Gilman Drive, La Jolla, CA 92093, USAClaude‐André Faucher‐GiguèreDepartment of Physics and Astronomy and CIERA, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USAEliot QuataertDepartment of Astronomy and Theoretical Astrophysics Center, University of California Berkeley, Berkeley, CA 94720, USAMichael Boylan-KolchinDepartment of Astronomy, The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712, USANorman MurrayCanadian Institute for Theoretical Astrophysics, 60 St. George Street, University of Toronto, ON M5S 3H8, CanadaChristopher C. HaywardCenter for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USAShea Garrison-KimmelTAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USACameron HummelsTAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USARobert FeldmannDepartment of Astronomy and Theoretical Astrophysics Center, University of California Berkeley, Berkeley, CA 94720, USAPaul TorreyDepartment of Physics, MIT, 77 Massachusetts Avenue, Cambridge, MA 02139, USAXiangcheng MaTAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USADaniel Anglés‐AlcázarDepartment of Physics and Astronomy and CIERA, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USAKung-Yi SuTAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USAM. OrrTAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USADenise SchmitzTAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USAIvanna EscalaTAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USARobyn E. SandersonTAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USAMichael Y GrudićTAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USAZachary HafenDepartment of Physics and Astronomy and CIERA, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USAJi-hoon KimKavli Institute for Particle Astrophysics and Cosmology, Department of Physics, Stanford University, Stanford, CA, USAAlex FittsDepartment of Astronomy, The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712, USAJames S. BullockDepartment of Physics and Astronomy, University of California, Irvine, CA 92697, USACoral WheelerTAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USAT K ChanDepartment of Physics, Center for Astrophysics and Space Science, University of California at San Diego, 9500 Gilman Drive, La Jolla, CA 92093, USAOliver D. ElbertDepartment of Physics and Astronomy, University of California, Irvine, CA 92697, USADesika NarayananDepartment of Astronomy, University of Florida, Gainesville, FL 32611, USA

2018en

ABI

Аннотация

The Feedback In Realistic Environments (FIRE) project explores feedback in cosmological galaxy formation simulations. Previous FIRE simulations used an identical source code ('FIRE-1') for consistency. Motivated by the development of more accurate numerics -including hydrodynamic solvers, gravitational softening, and supernova coupling algorithms -and exploration of new physics (e.g. magnetic fields), we introduce 'FIRE-2', an updated numerical implementation of FIRE physics for the gizmo code. We run a suite of simulations and compare against FIRE-1: overall, FIRE-2 improvements do not qualitatively change galaxy-scale properties. We pursue an extensive study of numerics versus physics. Details of the star formation algorithm, cooling physics, and chemistry have weak effects provided that we include metal-line cooling and star formation occurs at higher-than-mean densities. We present new resolution criteria for high-resolution galaxy simulations. Most galaxy-scale properties are robust to numerics we test, provided: (1) Toomre masses are resolved; (2) feedback coupling ensures conservation, and (3) individual supernovae are time-resolved. Stellar masses and profiles are most robust to resolution, followed by metal abundances and morphologies, followed by properties of winds and circum-galactic media. Central (kpc) mass concentrations in massive (>L*) galaxies are sensitive to numerics (via trapping/recycling of winds in hot haloes). Multiple feedback mechanisms play key roles: supernovae regulate stellar masses/winds; stellar mass-loss fuels late star formation; radiative feedback suppresses accretion on to dwarfs and instantaneous star formation in discs. We provide all initial conditions and numerical algorithms used.

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Идентификаторы

DOI: 10.1093/mnras/sty1690

Цитирования и источники

Цитирований: 4Использованных источников: 0

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