Gaseous Galaxy Halos

Abstract

Galactic halo gas traces inflowing star formation fuel and feedback from a galaxy's disk and is therefore crucial to our understanding of galaxy evolution. In this review, we summarize the multi-wavelength observational properties and origin models of Galactic and low redshift spiral galaxy halo gas. Galactic halos contain multiphase gas flows that are dominated in mass by the ionized component and extend to large radii. The densest, coldest halo gas observed in neutral hydrogen (HI) is generally closest to the disk (< 20 kpc), and absorption line results indicate warm and warm-hot diffuse halo gas is present throughout a galaxy's halo. The hot halo gas detected is not a significant fraction of a galaxy's baryons. The disk-halo interface is where the multiphase flows are integrated into the star forming disk, and there is evidence for both feedback and fueling at this interface from the temperature and kinematic gradient of the gas and HI structures. The origin and fate of halo gas is considered in the context of cosmological and idealized local simulations. Accretion along cosmic filaments occurs in both a hot (> 10^5.5 K) and cold mode in simulations, with the compressed material close to the disk the coldest and densest, in agreement with observations. There is evidence in halo gas observations for radiative and mechanical feedback mechanisms, including escaping photons from the disk, supernova-driven winds, and a galactic fountain. Satellite accretion also leaves behind abundant halo gas. This satellite gas interacts with the existing halo medium, and much of this gas will become part of the diffuse halo before it can reach the disk. The accretion rate from cold and warm halo gas is generally below a galaxy disk's star formation rate, but gas at the disk-halo interface and stellar feedback may be important additional fuel sources.

50 pages, 9 figures (1 in 3D, view with a current version of Adobe), to appear in ARA&A, 50, 491

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• Cold-mode and hot-mode accretion in galaxy formation: an entropy approach
• Distant probes of RM structure -- Where is the Faraday Rotation towards the Magellanic Leading Arm?
• Feeding the Dead: Neutral Gas Inflow in a Long-Quenched Ancient Massive Galaxy at $z\sim 2.7$ Observed with JWST/NIRSpec
• Introducing the Descriptive Parametric Model: Gaseous Profiles for Galaxies, Groups, and Clusters
• CGM cloud sizes from refractive FRB scattering
• The MeerKAT Absorption Line Survey (MALS) data release 3: Cold atomic gas associated with the Milky Way
• The effect of saturated thermal conduction on clouds in a hot plasma
• Accretion Onto the Milky Way: The Smith Cloud
• Fading in the Flow: Suppression of cold gas growth in expanding galactic outflows
• Neutral Gas Accretion onto Nearby Galaxies
• Extraplanar emission in isolated edge-on late-type galaxies. I. The H$\alpha$ distribution versus to the old and young stellar discs
• A path towards constraining the evolution of the interstellar medium and outflows in the Milky Way using APOGEE
• Hydrodynamics of Clustered Clouds: Drafting, Survival, Condensation, and Ablation
• Magnetising galaxies with cold inflows
• The WSRT HALOGAS Survey
• Atomic and Molecular Phases of the Interstellar Medium
• Cosmic Rays and Non-thermal Emission Induced by Accretion of Cool Gas onto the Galactic Disk
• The Discovery and Origin of A Very-High Velocity Cloud Toward M33
• Neural Infalling Cloud Equations (NICE): Increasing the Efficacy of Subgrid Models and Scientific Equation Discovery using Neural ODEs and Symbolic Regression
• Investigating Galactic Fountains in M101: Insights from Ionized, UV emissions and Neutral Gas
• Soft X-ray line emission from hot gas in intervening galaxy halos and diffuse gas in the cosmic web
• Interaction Between Rogue HI Clouds and the Magnetic Field High Above the Galaxy
• Game Theory in Cosmology
• How does the stellar disk of the Milky Way get its gas?
• Estimating the Fuel Supply Rate on the Galactic Disk from High Velocity Clouds (HVCs) Infall
• The Baryonic Mass Estimates of the Milky Way Halo in the form of High Velocity Clouds
• The Observed O VI is Just the Tip of the Iceberg: Estimating the Hidden Material in Circumgalactic and Intergalactic Clouds
• Resolving the formation of cold HI filaments in the high velocity cloud complex C
• A Search for OH 18-cm Emission from Intermediate-Velocity Gas at High Galactic Latitudes
• Atmospheric pressure and molecular cloud formation in early-type galaxies
• Kinematic analysis of an Ultra-Strong MgII absorber at z~1.13 linking to Circumgalactic Gas Structures
• Gamma rays from reaccelerated cosmic rays in high velocity clouds colliding with the Galactic disk
• Angular Momentum Accretion onto Disc Galaxies
• Constraints on cosmic rays in the Milky Way circumgalactic medium from OVIII observations
• The HaloSat and PolarLight CubeSat Missions for X-ray Astrophysics
• Simulating High-Velocity Clouds in the Observational Plane: An Initial Study with the Smith Cloud
• EMBERS I: Low redshift post-starburst galaxies are frequently depleted in molecular gas relative to star forming progenitors
• Modeling the Accretion of High-Velocity Clouds from a Rotating Halo
• Constraining the geometry of the gas surrounding a typical galaxy at $z=3.4$ with Ly$\alpha$ polarization