The physical drivers of the atomic hydrogen-halo mass relation

Abstract

We use SHARK, a semi-analytic galaxy formation model, to investigate the physical processes involved in dictating the shape, scatter and evolution of the HI-halo mass relation at $0\le z\le 2$. We compare SHARK with HI clustering and spectral stacking of the HI-halo mass relation derived from observations finding excellent agreement with the former and a deficiency of HI in SHARK at $M_{\mathrm{vir}}\approx 10^{12-13}{M}_{\odot }$ in the latter, but otherwise great agreement below and above that mass threshold. In SHARK, we find that the HI mass increases with the halo mass up to a critical mass of $\approx 10^{11.8}{M}_{\odot }$; between $\sim 10^{11.8}-10^{13}{M}_{\odot }$, the scatter in the relation increases by 0.7 dex and the HI mass decreases with the halo mass on average; at $M_{\mathrm{vir}}\ge 10^{13}{M}_{\odot }$, the HI content continues to increase with halo mass. We find that the critical halo mass of $\approx 10^{12}{M}_{\odot }$ is largely set by feedback from Active Galactic Nuclei (AGN), and the exact shape and scatter of the HI-halo mass relation around that mass is extremely sensitive to how AGN feedback is modelled, with other physical processes playing a less significant role. We determine the main secondary parameters responsible for the scatter of the HI-halo mass relation, namely the halo spin parameter at $M_{\mathrm{vir}}\le 10^{11.8}{M}_{\odot }$, and the fractional contribution from substructure to the total halo mass for $M_{\mathrm{vir}}\ge 10^{13}{M}_{\odot }$. The scatter at $10^{11.8}<M_{\mathrm{vir}}<10^{13}{M}_{\odot }$ is best described by the black-hole-to-stellar mass ratio of the central galaxy, reflecting the AGN feedback relevance. We present a numerical model to populate dark matter-only simulations with HI at $0\le z\le 2$ based solely on halo parameters that are measurable in such simulations.

Accepted for publication in MNRAS

References in corpus (27)

• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations
• The Role of Pressure in GMC Formation II: The H_2 - Pressure Relation
• A primer on hierarchical galaxy formation: the semi-analytical approach
• Halo assembly bias and its effects on galaxy clustering
• On the (Non)Evolution of HI Disks over Cosmic Time
• The Clustering of the SDSS Main Galaxy Sample II: Mock galaxy catalogues and a measurement of the growth of structure from Redshift Space Distortions at $z=0.15$
• Cold gas stripping in satellite galaxies: from pairs to clusters
• Corrfunc --- A Suite of Blazing Fast Correlation Functions on the CPU
• The origin of scatter in the stellar mass - halo mass relation of central galaxies in the EAGLE simulation
• Galaxy groups in the low-redshift Universe
• Atomic and molecular gas in IllustrisTNG galaxies at low redshift
• Variation of galactic cold gas reservoirs with stellar mass
• Hunting for Galaxies and Halos in simulations with VELOCIraptor
• Neutral hydrogen (HI) gas content of galaxies at $z\approx 0.32$
• The origin of the atomic and molecular gas contents of early-type galaxies. I. A new test of galaxy formation physics
• The Clustering Characteristics of HI-Selected Galaxies from the 40% ALFALFA Survey
• SURFS: Riding the waves with Synthetic UniveRses For Surveys
• The Weak Clustering of Gas-Rich Galaxies
• Constraining the HI-Halo Mass Relation From Galaxy Clustering
• Physical drivers of galaxies' cold-gas content: exploring environmental and evolutionary effects with DARK SAGE
• Black hole spin and radio loudness in a LCDM universe
• Direct Measurement of the HI-Halo Mass Relation through Stacking
• The impact of stellar and AGN feedback on halo-scale baryonic and dark matter accretion in the EAGLE simulations
• An accurate low-redshift measurement of the cosmic neutral hydrogen density
• The first Super Massive Black Holes: indications from models for future observations
• The Baryonic Collapse Efficiency of Galaxy Groups in the RESOLVE and ECO Surveys

Cited by in corpus (4)

• The galaxy HI-(sub)halo connection and the HI spatial clustering of local galaxies
• Galaxy And Mass Assembly (GAMA): The group HI mass as a function of halo mass
• The variation of the gas content of galaxy groups and pairs compared to isolated galaxies
• HI HOD -- I. The Halo Occupation Distribution of HI Galaxies