EDGE: What shapes the relationship between H <scp>i</scp> and stellar observables in faint dwarf galaxies?
Martin P. Rey, Andrew Pontzen, Oscar Agertz, Matthew D A Orkney, Justin I. Read, A. Saintonge, Stacy Y. Kim, Payel Das
Abstract
ABSTRACT We show how the interplay between feedback and mass-growth histories introduces scatter in the relationship between stellar and neutral gas properties of field faint dwarf galaxies ($M_{\star }\lessapprox 10^{6} \, \mbox{M}_\mathrm{\odot }$). Across a suite of cosmological, high-resolution zoomed simulations, we find that dwarf galaxies of stellar masses $10^5 \le M_{\star }\le 10^{6} \, \mbox{M}_\mathrm{\odot }$ are bimodal in their cold gas content, being either H i-rich or H i-deficient. This bimodality is generated through the coupling between (i) the modulation of H i contents by the background of ultraviolet radiation (UVB) at late times and (ii) the significant scatter in the stellar-to-halo mass relationship induced by reionization. Furthermore, our H i-rich dwarfs exhibit disturbed and time-variable neutral gas distributions primarily due to stellar feedback. Over the last four billion years, we observe order-of-magnitude changes around the median $M_{\mathrm{H\,\small {I} }}$, factor-of-a-few variations in H i spatial extents, and spatial offsets between H i and stellar components regularly exceeding the galaxies’ optical sizes. Time variability introduces further scatter in the $M_{\star }\!-\! M_{\mathrm{H\,\small {I} }}$ relation and affects a galaxy’s detectability in H i at any given time. These effects will need to be accounted for when interpreting observations of the population of faint, H i-bearing dwarfs by the combination of optical and radio wide, deep surveys.