A Unified Model for the Coevolution of Galaxies and Their Circumgalactic Medium: The Relative Roles of Turbulence and Atomic Cooling Physics

Viraj Pandya*, Drummond B. Fielding, Greg L. Bryan, Christopher Carr, Rachel S. Somerville, Jonathan Stern, Claude André Faucher-Giguère, Zachary Hafen, Daniel Anglés-Alcázar, John C. Forbes

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

4 Scopus citations

Abstract

The circumgalactic medium (CGM) plays a pivotal role in regulating gas flows around galaxies and thus shapes their evolution. However, the details of how galaxies and their CGM coevolve remain poorly understood. We present a new time-dependent two-zone model that self-consistently tracks not just mass and metal flows between galaxies and their CGM but also the evolution of the global thermal and turbulent kinetic energy of the CGM. Our model accounts for heating and turbulence driven by both supernova winds and cosmic accretion as well as radiative cooling, turbulence dissipation, and halo outflows due to CGM overpressurization. We demonstrate that, depending on parameters, the CGM can undergo a phase transition (“thermalization”) from a cool, turbulence-supported phase to a virial-temperature, thermally supported phase. This CGM phase transition is largely determined by the ability of radiative cooling to balance heating from supernova winds and turbulence dissipation. We perform an initial calibration of our model to the FIRE-2 cosmological hydrodynamical simulations and show that it can approximately reproduce the baryon cycles of the simulated halos. In particular, we find that, for these parameters, the phase transition occurs at high redshift in ultrafaint progenitors and at low redshift in classical M vir ∼ 1011 M dwarfs, while Milky Way-mass halos undergo the transition at z ≈ 0.5. We see a similar transition in the simulations though it is more gradual, likely reflecting radial dependence and multiphase gas not captured by our model. We discuss these and other limitations of the model and possible future extensions.

Original languageEnglish
Article number118
JournalAstrophysical Journal
Volume956
Issue number2
DOIs
StatePublished - 1 Oct 2023

Funding

FundersFunder number
CXOTM2-23005X
XSEDEAST-1715216, AST-2108230, 17-ATP17-0067, 822237, 21-ATP21-0036, AST-1652522, 80NSSC21K1053, MCA06N030
National Science FoundationAST-2108470
National Aeronautics and Space AdministrationHST-HF2-51489
Simons Foundation
Research Corporation for Science AdvancementAST-2108944, AST-2009687, TM2-23006X, CCA-1018464
Space Telescope Science InstituteHST-GO-16730.016-A, NAS5-26555, HST-AR-16124.001-A
Israel Science Foundation2584/21

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