Cited by 76Galaxies: Formation, Evolution, PhenomenaAstrophysics and Star Formation StudiesStellar, planetary, and galactic studies

Properties of H i discs in the Auriga cosmological simulations

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Marinacci, Federico, Grand, Robert J. J., Pakmor, Rüdiger, Springel, Volker, Gómez, Facundo A., Frenk, Carlos S., White, Simon D. M.·2017·Monthly Notices of the Royal Astronomical Society

Abstract

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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Crossref · 10.1093/mnras/stw3366

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  • The Auriga simulations successfully reproduce many properties of observed central and satellite galaxies, such as stellar masses and star formation rates of spirals, density and kinematics of stellar haloes, and the luminosity function of MW satellites.

    “The Auriga simulations successfully reproduce many properties of observed central and satellite galaxies, such as the stellar masses and star formation rates of spirals (Grand et al. 2017; Marinacci et al. 2017), the density and kinematics of stellar haloes (Deason et al. 2017; Monachesi et al. 2019b), and the luminosity function of MW satellites (Simpson et al. 2018).”

    From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Marinacci et al. 2017

    The Abstract (p. 1) says Auriga forms realistic late-type galaxies, and §4.6 (p. 14) compares their H I gas fractions across stellar masses with observations. But the Marinacci et al. citation is attached specifically to the claim that spiral galaxies’ stellar masses and star formation rates match observations; the passages found do not establish those two comparisons. The stellar-halo and satellite claims have separate citations and are not assessed here. (LLM, conf=0.74)

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Research works printed but not linked: 4

  1. Crain R. A., et al., 2016, preprint, ( arXiv:1604.06803 ) · arXiv
  2. G´ omez F. A., White S. D. M., Grand R. J. J., Marinacci F., Springel V., Pakmor R., 2016a, preprint, ( arXiv:1606.06295 ) · arXiv
  3. Grand R. J. J., et al., 2016a, preprint, ( arXiv:1610.01159 ) · arXiv
  4. Powell K. G., Roe P. L., Linde T. J., Gombosi T. I., De Zeeuw D. L., 1999, Journal of Computational Physics, 154, 284

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Authors
Marinacci, F., Grand, R. J. J., Pakmor, R., Springel, V., Gómez, F. A., Frenk, C. S., & White, S. D. M.
Affiliations
  • Massachusetts Institute of Technology (US)
  • Heidelberg University (DE)
  • Heidelberg Institute for Theoretical Studies (DE)
  • Max Planck Institute for Astrophysics (DE)
  • Durham University (GB)
Corresponding author
Marinacci, Federico
Venue
Monthly Notices of the Royal Astronomical Society
Published
2017-01-18
Volume
466
Issue
4
Pages
3859-3875
ISSN
  • 0035-8711 (ISSN-L)
  • 1365-2966
OpenAlex
W2528377752
Cited by
75
References
113
Citations by year
2026: 6 · 2025: 8 · 2024: 7 · 2023: 6 · 2022: 6 · 2021: 7 · 2020: 14 · 2019: 11 · 2018: 5 · 2017: 5
FWCI
3.35
Type
journal article
Language
en
Open access
Locations
  • Monthly Notices of the Royal Astronomical Society (publishedVersion)
  • arXiv (Cornell University) (publishedVersion)
  • Durham Research Online (Durham University) (acceptedVersion)
  • Liverpool John Moores University (acceptedVersion)
  • Durham Research Online (Durham University) (submittedVersion, cc-by)
  • Archivio istituzionale della ricerca (Alma Mater Studiorum Università di Bologna) (submittedVersion)
  • Max Planck Digital Library (submittedVersion)
  • MPG.PuRe (Max Planck Society) (submittedVersion)
  • arXiv (Cornell University)
Funders
ERC (EXAGAL-308037)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
Keywords
neutral hydrogen, HI discs, Auriga simulations, late-type galaxies, star formation rate, galaxy formation

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