Journal
ASTROPHYSICAL JOURNAL
Volume 905, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/1538-4357/abc3c1
Keywords
Galaxy formation; Galactic winds; Galaxy evolution; Circumgalactic medium; Dwarf galaxies; Galaxy dark matter halos; Hydrodynamical simulations; Analytical mathematics; Star formation
Categories
Funding
- Center for Computational Astrophysics at the Flatiron Institute
- Simons Foundation
- National Science Foundation Graduate Research Fellowship Program [1339067]
- NSF [AST-1615955, OAC-1835509]
- NASA [NNX15AB20G]
- NASA ATP [NNX17AG26G]
- Simons Foundation [CCA 528307]
- Division Of Graduate Education
- Direct For Education and Human Resources [1339067] Funding Source: National Science Foundation
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Semianalytic models (SAMs) are a promising means of tracking the physical processes associated with galaxy formation, but many of their approximations have not been rigorously tested. As part of the Simulating Multiscale Astrophysics to Understand Galaxies project, we compare predictions from the FIRE-2 hydrodynamical zoom-in simulations to those from the Santa Cruz SAM run on the same halo merger trees, with an emphasis on the global mass flow cycle. Our study includes 13 halos spanning low-mass dwarfs (M-vir similar to 10(10)M at z = 0), intermediate-mass dwarfs (M-vir similar to 10(11)M), and Milky Way-mass galaxies (M-vir similar to 10(12)M). The SAM and FIRE-2 predictions agree relatively well with each other in terms of stellar and interstellar medium mass but differ dramatically on circumgalactic medium mass (the SAM is lower than FIRE-2 by similar to 3 orders of magnitude for dwarfs). Strikingly, the SAM predicts higher gas accretion rates for dwarfs compared to FIRE-2 by factors of similar to 10-100, and this is compensated for with higher mass outflow rates in the SAM. We argue that the most severe model discrepancies are caused by the lack of preventative stellar feedback and the assumptions for halo gas cooling and recycling in the SAM. As a first step toward resolving these model tensions, we present a simple yet promising new preventative stellar feedback model in which the energy carried by supernova-driven winds is allowed to heat some fraction of gas outside of halos to at least the virial temperature such that accretion is suppressed.
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