Methods: numerical, stars: formation, galaxies: active, galaxies: evolution, galaxies: formation, cosmology: theory 1 INTRODUCTIONįeedback from stars is an essential and still poorly understood component of galaxy formation. We provide all initial conditions and numerical algorithms used. 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. Central (∼kpc) mass concentrations in massive (> L *) galaxies are sensitive to numerics (via trapping/recycling of winds in hot haloes). Stellar masses and profiles are most robust to resolution, followed by metal abundances and morphologies, followed by properties of winds and circum-galactic media. 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. We present new resolution criteria for high-resolution galaxy simulations. 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 pursue an extensive study of numerics versus physics. We run a suite of simulations and compare against FIRE-1: overall, FIRE-2 improvements do not qualitatively change galaxy-scale properties. magnetic fields), we introduce ‘FIRE-2’, an updated numerical implementation of FIRE physics for the gizmo code. Motivated by the development of more accurate numerics – including hydrodynamic solvers, gravitational softening, and supernova coupling algorithms – and exploration of new physics (e.g. Previous FIRE simulations used an identical source code (‘FIRE-1’) for consistency. The Feedback In Realistic Environments (FIRE) project explores feedback in cosmological galaxy formation simulations.
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