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.

arXiv commentAccepted for publication in MNRAS

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