Cited by 557Galaxies: Formation, Evolution, PhenomenaAstrophysics and Star Formation StudiesAstrophysical Phenomena and Observations

The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time

Open access
Grand, Robert J. J., Gómez, Facundo A., Marinacci, Federico, Pakmor, Rüdiger, Springel, Volker, Campbell, David J. R., Frenk, Carlos S., Jenkins, Adrian +1 more·2017·Monthly Notices of the Royal Astronomical Society

Abstract

We introduce a suite of 30 cosmological magneto-hydrodynamical zoom simulations of the formation of galaxies in isolated Milky Way mass dark haloes. These were carried out with the moving mesh code arepo, together with a comprehensive model for galaxy formation physics, including active galactic nuclei (AGN) feedback and magnetic fields, which produces realistic galaxy populations in large cosmological simulations. We demonstrate that our simulations reproduce a wide range of present-day observables, in particular, two-component disc-dominated galaxies with appropriate stellar masses, sizes, rotation curves, star formation rates and metallicities. We investigate the driving mechanisms that set present-day disc sizes/scalelengths, and find that they are related to the angular momentum of halo material. We show that the largest discs are produced by quiescent mergers that inspiral into the galaxy and deposit high-angular momentum material into the pre-existing disc, simultaneously increasing the spin of dark matter and gas in the halo. More violent mergers and strong AGN feedback play roles in limiting disc size by destroying pre-existing discs and by suppressing gas accretion on to the outer disc, respectively. The most important factor that leads to compact discs, however, is simply a low angular momentum for the halo. In these cases, AGN feedback plays an important role in limiting central star formation and the formation of a massive bulge.

The claims and statistics of this paper haven’t been checked yet.

Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.

A few free checks a day · papers already verified open instantly · results are public

Integrity signals

Registry

Crossref · 10.1093/mnras/stx071

Cites

133 of 133 references verified0 citation errors · 0 not checkable

Statistics

Claims the paper makes

The claims and statistics of this paper haven’t been checked yet.

Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.

A few free checks a day · papers already verified open instantly · results are public

Claims other papers make about this one

Each is checked against this paper’s own text: does it say what the citing paper says it does?

  • The Auriga suite consists of 40 haloes, 30 of which have mass M_200 ∈ [1,2] × 10^12 M_sun, plus 10 additional lower mass haloes with M_200 just below ∼10^12 M_sun.

    “The suite consist of 40 haloes, 30 of which have mass, M 200 ∈ [1 , 2] × 10 12 M ⊙ , and were first introduced in Grand et al. (2017), plus 10 additional lower mass haloes, with M 200 masses just below ∼ 10 12 M ⊙”

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

    Section 2.1 says Auriga comprises 30 haloes, and Section 2.2 gives their selection range as 1 < M_200/10^12 M_sun < 2. The paper does not report a 40-halo suite or the 10 additional lower-mass haloes, so it supports only the original 30-halo portion of the claim. (LLM, conf=0.88)

    Experimental — accuracy not yet measured
  • 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 Grand et al. 2017

Self-check

Percentages, sums and reported differences re-computed from the paper’s own numbers.

The self-check needs the paper’s full text.

Cites

Flagged first, then by citations

Research works printed but not linked: 2

  1. Marinacci F., Grand R., Pakmor R., Springel V., Gómez F., Frenk C., White S., 2016, MNRAS, preprint (arXiv:1610.01594) · arXiv
  2. Torrey P., Wellons S., Ma C.-P., Hopkins P. F., Vogelsberger M., 2016, preprint (arXiv:1606.07271) · arXiv

Cited by

Sorted by citations

Authors
Grand, R. J. J., Gómez, F. A., Marinacci, F., Pakmor, R., Springel, V., Campbell, D. J. R., Frenk, C. S., Jenkins, A., & White, S. D. M.
Affiliations
  • Heidelberg University (DE)
  • Max Planck Institute for Astrophysics (DE)
  • Massachusetts Institute of Technology (US)
  • Heidelberg Institute for Theoretical Studies (DE)
  • Durham University (GB)
Corresponding author
Grand, Robert J. J.
Venue
Monthly Notices of the Royal Astronomical Society
Published
2017-01-12
Pages
stx071
ISSN
  • 0035-8711 (ISSN-L)
  • 1365-2966
OpenAlex
W2528641579
Cited by
557
References
133
Citations by year
2026: 33 · 2025: 74 · 2024: 61 · 2023: 65 · 2022: 81 · 2021: 55 · 2020: 69 · 2019: 62 · 2018: 35 · 2017: 20 · 2016: 1 · 2015: 1
FWCI
27.82
Type
journal article
Language
en
Open access
Locations
  • Monthly Notices of the Royal Astronomical Society (publishedVersion)
  • Durham Research Online (Durham University) (acceptedVersion)
  • Liverpool John Moores University (acceptedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • Archivio istituzionale della ricerca (Alma Mater Studiorum Università di Bologna) (submittedVersion, other-oa)
  • Durham Research Online (Durham University) (submittedVersion, cc-by)
  • MPG.PuRe (Max Planck Society) (submittedVersion)
  • arXiv (Cornell University)
Funders
  • Durham University (ST/K00042X/1, ST/K003267/1, ST/H008519/1)
  • Deutsche Forschungsgemeinschaft
  • Gauss Centre for Supercomputing
  • Science and Technology Facilities Council (ST/H008519, ST/K00042X/1, ST/I00162X/1, ST/L00075X/1, ST/M007006/1, ST/P000541/1, ST/I001573/1, ST/H008519/1, ST/K003267/1)
  • Leibniz-Gemeinschaft
  • FP7 Ideas: European Research Council (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 › Astrophysical Phenomena and Observations
Keywords
disk galaxies, galaxy formation, zoom-in simulations, AGN feedback, magnetic field, angular momentum, disk size, dark matter halos, bulge formation, star formation rate, metallicity, rotation curves, gas accretion

About these checks

Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.

Statistics and arithmetic are recomputed, not judged.

Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.

What counts as a claim ›How we measure confidence ›How we check this ›

Are you an author, or do you see a problem with this page? Request a review