XGASS: the scatter of the H i–halo mass relation of central galaxies

Abstract

ABSTRACT Empirical studies of the relationship between baryonic matter in galaxies and the gravitational potential of their host haloes are important to constrain our theoretical framework for galaxy formation and evolution. One such relation, between the atomic hydrogen (H i) mass of central galaxies (MH i,c) and the total mass of their host haloes (Mhalo), has attracted significant interest in the last few years. In this work, we use the extended GALEX Arecibo SDSS Survey to examine the scatter of the H i–halo mass relation for a representative sample of central galaxies. Our findings reveal a flat median relation at $\mathrm{ log}_{10}(M_{\rm {H\,{\small I},c}}/\rm {M}_{\odot }) \approx 9.40$, across $11.1 \lt \mathrm{ log}_{10}(M_{\rm {halo}}/{{\rm M}_{\odot }}) \lt 14.1$. This flat relation stems from the statistical dominance of star-forming, disc galaxies at low Mhalo in combination with the increasing prevalence of passive, high stellar concentration systems at higher Mhalo. The scatter of this relation and the stellar specific angular momentum of centrals have a strong link (Spearman’s rank correlation coefficient ≥0.5). Comparisons with simulations suggest that the kinematic state of host haloes may be primarily driving this scatter. Our findings highlight that the H i–halo mass parameter space is too complex to be completely represented by simple median or average relations and we show that tensions with previous works are most likely due to selection biases. We recommend that future observational studies, and their comparisons with theoretical models, bin central galaxies also by their secondary properties to enable a statistically robust understanding of the processes regulating the cold gas content within central galaxies of dark matter haloes.