EDGE: What shapes the relationship between H i and stellar observables in faint dwarf galaxies?. Issue 4 (25th February 2022)

• Record Type: Journal Article
• Authors: Rey, Martin P; Pontzen, Andrew; Agertz, Oscar; Orkney, Matthew D A; Read, Justin I; Saintonge, Amélie; Kim, Stacy Y; Das, Payel
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 511:Issue 4(2022)
• Page Start: 5672
• Page End: 5681
• Publication Date: 2022-02-25
• Subjects: methods: numerical -- galaxies: dwarf -- galaxies: evolution -- galaxies: haloes -- galaxies: structure; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stac502
• Languages: English
• ISSNs: 0035-8711

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.