2016/08/31 by Hamsa Padmanabhan, Girish Kulkarni
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Galactic halo #Galaxies: Formation, Evolution, Phenomena #Galaxy #Gamma-ray bursts and supernovae #Halo #Physics #astro-ph.CO #astro-ph.GA
paper · pdf · doi:10.1093/mnras/stx1178
published as MNRAS, Volume 470, Issue 1, p.340-349 (2017) · 11 pages, 8 figures, 1 table; published in MNRAS. v3: minor typo corrected; results unchanged
openalex created_date 2016/08/23 · openalex publication_date 2017/05/12 · arxiv created 2017/07/19 · arxiv updated 2017/08/23 · openalex updated_date 2026/08/05
The neutral hydrogen (H i) content of dark matter haloes forms an intermediate state in the baryon cycle that connects the hot shock-heated gas and cold star-forming gas in haloes. Measurement of the relationship between H i mass and halo mass therefore puts important constraints on galaxy formation models. We combine radio observations of H i in emission at low redshift (z ∼ 0) with optical/UV observations of H i in absorption at high redshift (1 < z < 4) to derive constraints on the evolution of the H i-mass–halo-mass (HIHM) relation from redshift z = 4 to 0. We find that one can model the HIHM relation similar to the stellar-mass–halo-mass (SHM) relation at z ∼ 0. At z = 0, haloes with mass 1011.7 M⊙ have the highest H i mass fraction (∼1 per cent), which is about four times smaller than their stellar-mass fraction. We model the evolution of the HIHM relation in a manner similar to that of the SHM relation. Combining this parametrization with a redshift- and mass-dependent modified Navarro–Frenk–White profile for the H i density within a halo, we draw constraints on the evolution of the HIHM relation from the observed H i column density, incidence rate and clustering bias at high redshift. We compare these findings with results from hydrodynamical simulations and other approaches in the literature and find the models to be consistent with each other at the 68 per cent confidence level.