The Compression of Dark Matter Halos by Baryonic Infall
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The initial radial density profiles of dark matter halos are laid down by gravitational collapse in hierarchical structure formation scenarios and are subject to further compression as baryons cool and settle to the halo centers. Here we describe an explicit implementation of the algorithm, originally developed by Young, to calculate changes to the density profile as the result of adiabatic infall in a spherical halo model. Halos with random motion are more resistant to compression than are those in which random motions are neglected, which is a key weakness of the simple method widely employed. Young's algorithm results in density profiles in excellent agreement with those from N -body simulations. We show how the algorithm can be applied to determine the original uncompressed halos of real galaxies, a step that must be computed with care in order to enable a confrontation with theoretical predictions from theories such as ΛCDM.
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The response of the DM halo to the assembly of its galaxy can be predicted to good approximation using the adiabatic contraction method with same action integrals.
“The response of the DM halo to the assembly of its galaxy can be predicted to good approximation using the adiabatic contraction method in which the DM distribution is assumed to have the same action integrals in the hydrodynamic run as in the DMO case (Sellwood & McGaugh 2005; Callingham et al. 2020”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Sellwood & McGaugh 2005
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A Philosophical Approach to MOND: Assessing the Milgromian Research Program in CosmologyPreprint
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Self-citation
- Authors
- Sellwood, J. A., & McGaugh, S. S.
- Affiliations
- Rutgers, The State University of New Jersey (US)
- University of Maryland, College Park (US)
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2005-11-20
- Volume
- 634
- Issue
- 1
- Pages
- 70-76
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2023518980
- Cited by
- 164
- References
- 61
- Citations by year
- 2026: 3 · 2025: 6 · 2024: 3 · 2023: 8 · 2022: 4 · 2021: 7 · 2020: 19 · 2019: 5 · 2018: 4 · 2017: 1 · 2016: 6 · 2015: 8 · 2014: 12 · 2013: 7 · 2012: 8
- FWCI
- 6.40
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- Scholarly Commons @ Case Western Reserve University (submittedVersion)
- CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Dark Matter and Cosmic Phenomena
- Keywords
- dark matter halos, halo density profiles, hierarchical structure formation, random motion, galaxy halos
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