Origin of the galaxy H I size-mass relation
We analytically derive the observed size-mass relation of galaxies’ atomic hydrogen (H i), including limits on its scatter, based on simple assumptions about the structure of H i discs. We trial three generic profiles for H i surface density as a function of radius. First, we assert that H i surface...
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| Hauptverfasser: | , , , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
2019 September 10
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2019, Jahrgang: 490, Heft: 1, Pages: 96-113 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stz2513 |
| Online-Zugang: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1093/mnras/stz2513
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| Verfasserangaben: | Adam R.H. Stevens, Benedikt Diemer, Claudia del P. Lagos, Dylan Nelson, Danail Obreschkow, Jing Wang and Federico Marinacci |
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| 100 | 1 | |a Stevens, Adam R. H. |e VerfasserIn |0 (DE-588)1252333757 |0 (DE-627)1793487006 |4 aut | |
| 245 | 1 | 0 | |a Origin of the galaxy H I size-mass relation |c Adam R.H. Stevens, Benedikt Diemer, Claudia del P. Lagos, Dylan Nelson, Danail Obreschkow, Jing Wang and Federico Marinacci |
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| 520 | |a We analytically derive the observed size-mass relation of galaxies’ atomic hydrogen (H i), including limits on its scatter, based on simple assumptions about the structure of H i discs. We trial three generic profiles for H i surface density as a function of radius. First, we assert that H i surface densities saturate at a variable threshold, and otherwise fall off exponentially with radius or, secondly, radius squared. Our third model assumes the total gas surface density is exponential, with the H i fraction at each radius depending on local pressure. These are tested against a compilation of 110 galaxies from the THINGS, LITTLE THINGS, LVHIS, and Bluedisk surveys, whose H i surface density profiles are well resolved. All models fit the observations well and predict consistent size-mass relations. Using an analytical argument, we explain why processes that cause gas disc truncation - such as ram-pressure stripping - scarcely affect the H i size-mass relation. This is tested with the IllustrisTNG(100) cosmological, hydrodynamic simulation and the Dark Sage semi-analytic model of galaxy formation, both of which capture radially resolved disc structure. For galaxies with $m_* \ge 10^9\, {\rm M}_{\odot }$ and $m_{\rm H\, {\small {I}}} \ge 10^8\, {\rm M}_{\odot }$, both simulations predict H i size-mass relations that align with observations, show no difference between central and satellite galaxies, and show only a minor, second-order dependence on host halo mass for satellites. Ultimately, the universally tight H i size-mass relation is mathematically inevitable and robust. Only by completely disrupting the structure of H i discs, e.g. through overly powerful feedback, could a simulation predict the relation poorly. | ||
| 700 | 1 | |a Diemer, Benedikt |e VerfasserIn |0 (DE-588)1263698271 |0 (DE-627)1811812767 |4 aut | |
| 700 | 1 | |a Lagos, Claudia del P |e VerfasserIn |4 aut | |
| 700 | 1 | |a Nelson, Dylan |e VerfasserIn |0 (DE-588)115182805X |0 (DE-627)101233600X |0 (DE-576)42382581X |4 aut | |
| 700 | 1 | |a Obreschkow, Danail |e VerfasserIn |4 aut | |
| 700 | 1 | |a Wang, Jing |e VerfasserIn |4 aut | |
| 700 | 1 | |a Marinacci, Federico |e VerfasserIn |4 aut | |
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