Impact of baryon physics on dark matter structures: a detailed simulation study of halo density profiles: Baryonic back-reaction
Open accessAbstract
The back-reaction of baryons on the dark matter halo density profile is of great interest, not least because it is an important systematic uncertainty when attempting to detect the dark matter. Here, we draw on a large suite of high-resolution cosmological hydrodynamical simulations to systematically investigate this process and its dependence on the baryonic physics associated with galaxy formation. The effects of baryons on the dark matter distribution are typically not well described by adiabatic contraction models. In the inner 10 per cent of the virial radius the models are only successful if we allow their parameters to vary with baryonic physics, halo mass and redshift, thereby removing all predictive power. On larger scales the profiles from dark matter only simulations consistently provide better fits than adiabatic contraction models, even when we allow the parameters of the latter models to vary. The inclusion of baryons results in significantly more concentrated density profiles if radiative cooling is efficient and feedback is weak. The dark matter halo concentration can in that case increase by as much as 30 (10) per cent on galaxy (cluster) scales. The most significant effects occur in galaxies at high redshift, where there is a strong anticorrelation between the baryon fraction in the halo centre and the inner slope of both the total and the dark matter density profiles. If feedback is weak, isothermal inner profiles form, in agreement with observations of massive, early-type galaxies. However, we find that active galactic nuclei (AGN) feedback, or extremely efficient feedback from massive stars, is necessary to match observed stellar fractions in groups and clusters, as well as to keep the maximum circular velocity similar to the virial velocity as observed for disc galaxies. These strong feedback models reduce the baryon fraction in galaxies by a factor of 3 relative to the case with no feedback. The AGN is even capable of reducing the baryon fraction by a factor of 2 in the inner region of group and cluster haloes. This in turn results in inner density profiles which are typically shallower than isothermal and the halo concentrations tend to be lower than in the absence of baryons. We therefore conclude that the disagreement between the concentrations inferred from observations of groups of galaxies and predictions from simulations that was identified by Duffy et al. is not alleviated by the inclusion of baryons.
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The response of the DM halo to the baryonic component depends on galaxy assembly history.
“The response of the DM halo to the baryonic component depends on the galaxy assembly history (e.g. Duffy et al. 2010; Dutton et al. 2016; Artale et al. 2019)”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Duffy et al. 2010
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McMillan, P. J. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2759 · Cited by 1,099 · see citing works
The milky way total mass profile as inferred from Gaia DR2
Cautun, M., Benítez-Llambay, A., Deason, A. J., Frenk, C. S., Fattahi, A., Gómez, F. A., Grand, R. J. J., Oman, K. A., Navarro, J. F., & Simpson, C. M. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1017 · Cited by 332 · see citing works
“The response of the DM halo to the baryonic component depends on the galaxy assembly history (e.g. Duffy et al. 2010; Dutton et al. 2016; Artale et al. 2019); the good agreement between the halo contraction predictions in our three simulations suites reflects the fact that these simulations have…”
BackgroundMethodThe Milky Way total mass profile as inferred from Gaia DR2
Cautun, M., Benitez-Llambay, A., Deason, A. J., Frenk, C. S., Fattahi, A., Gómez, F. A., Grand, R. J. J., Oman, K. A., Navarro, J. F., & Simpson, C. M. (2019) · arXiv · doi:10.48550/arxiv.1911.04557 · Cited by 335
Dutton, A. A., Macciò, A. V., Dekel, A., Wang, L., Stinson, G., Obreja, A., Di Cintio, A., Brook, C., Buck, T., & Kang, X. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1537 · Cited by 100 · see citing works
A gradient based method for modeling baryons and matter in halos of fast simulations
Dai, B., Feng, Y., & Seljak, U. (2018) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2018/11/009 · Cited by 35 · see citing works
“Comparing to dark-matter-only simulation, AGN feedback in hydrodynamical simulation moves a large amount of gas from the center of halos to large radii [8, 10].”
Background
- Authors
- Duffy, A. R., Schaye, J., Kay, S. T., Vecchia, C. D., Battye, R. A., & Booth, C. M.
- Affiliations
- Leiden University (NL)
- University of Manchester (GB)
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2010-04
- Pages
- no-no
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W1881870510
- Cited by
- 186
- References
- 91
- Citations by year
- 2026: 8 · 2025: 14 · 2024: 15 · 2023: 15 · 2022: 13 · 2021: 13 · 2020: 21 · 2019: 14 · 2018: 12 · 2017: 7 · 2016: 14 · 2015: 10 · 2014: 5 · 2013: 7 · 2012: 12
- FWCI
- 4.47
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- UWA Profiles and Research Repository (UWA) (submittedVersion, other-oa)
- HighWire Press Open Archive (submittedVersion)
- Swinburne figshare (Swinburne University of Technology) (submittedVersion)
- arXiv (Cornell University)
- Funders
- European Science Foundation
- Ministry of Education, Culture, Sports, Science and Technology
- Nederlandse Organisatie voor Wetenschappelijk Onderzoek
- Virgo Consortium
- Science and Technology Facilities Council (ST/G002592/1)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Dark Matter and Cosmic Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
- Keywords
- halo density profiles, galaxy formation, AGN feedback, stellar feedback, radiative cooling, halo concentration, baryon fraction, early-type galaxies, galaxy groups and clusters, disk galaxies, cosmological hydrodynamical simulations
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.
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