Properties of HI discs in the Auriga cosmological simulations
We analyse the properties of the H i gas distribution in the Auriga project, a set of magnetohydrodynamic cosmological simulations performed with the moving-mesh code arepo and a physics model for galaxy formation that succeeds in forming realistic late-type galaxies in the 30 Milky Way-sized haloes...
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| Hauptverfasser: | , , , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
2017 January 18
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2017, Jahrgang: 466, Heft: 4, Pages: 3859-3875 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stw3366 |
| Online-Zugang: | Verlag, kostenfrei, Volltext: http://dx.doi.org/10.1093/mnras/stw3366
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| Verfasserangaben: | Federico Marinacci, Robert J.J. Grand, Rüdiger Pakmor, Volker Springel, Facundo A. Gómez, Carlos S. Frenk and Simon D.M. White |
MARC
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| 245 | 1 | 0 | |a Properties of HI discs in the Auriga cosmological simulations |c Federico Marinacci, Robert J.J. Grand, Rüdiger Pakmor, Volker Springel, Facundo A. Gómez, Carlos S. Frenk and Simon D.M. White |
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| 520 | |a We analyse the properties of the H i gas distribution in the Auriga project, a set of magnetohydrodynamic cosmological simulations performed with the moving-mesh code arepo and a physics model for galaxy formation that succeeds in forming realistic late-type galaxies in the 30 Milky Way-sized haloes simulated in this project. We use a simple approach to estimate the neutral hydrogen fraction in our simulation set, which treats low-density and star-forming gas separately, and we explore two different prescriptions to subtract the contribution of molecular hydrogen from the total H i content. The H i gas in the vast majority of the systems forms extended discs although more disturbed morphologies are present. Notwithstanding the general good agreement with observed H i properties - such as radial profiles and the mass-diameter relation - the Auriga galaxies are systematically larger and more gas-rich than typical nearby galaxies. Interestingly, the amount of H i gas outside the disc plane correlates with the star formation rate, consistent with a picture where most of this extra-planar H i gas originates from a fountain-like flow. Our findings are robust with respect to the different assumptions adopted for computing the molecular hydrogen fraction and do not vary significantly over a wide range of numerical resolution. The H i modelling introduced in this paper can be used in future work to build artificial interferometric H i data cubes, allowing an even closer comparison of the gas dynamics in simulated galaxies with observations. | ||
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