期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 480, 期 1, 页码 800-863出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sty1690
关键词
methods: numerical; stars: formation; galaxies: active; galaxies: evolution; galaxies: formation; cosmology: theory
资金
- Alfred P. Sloan Research Fellowship
- NASA ATP [NNX14AH35G]
- NSF [1715847, 1455342, AST-1412836, AST-1517491, AST-1517226, AST1412153, PRAC NSF.1713353]
- Caltech-Carnegie Fellowship
- Moore Center for Theoretical Cosmology and Physics at Caltech
- NASA [NNX15AB22G]
- Simons Foundation
- NASA through HST by STScI [AR-12836, AR-13888, AR-13896, AR-14282]
- Cottrell Scholar Award from the Research Corporation for Science Advancement
- Swiss National Science Foundation [157591]
- NASA HEC Program through the NAS Division at Ames Research Center
- NCCS at Goddard Space Flight Center
- Direct For Mathematical & Physical Scien [1517226, 1412153] Funding Source: National Science Foundation
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 (similar to 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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