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Cited by 764Galaxies: Formation, Evolution, PhenomenaCosmology and Gravitation TheoriesStellar, planetary, and galactic studies

The statistics of CDM halo concentrations

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Neto, A. F., Gao, L., Bett, P., Cole, S., Navarro, J. F., Frenk, C. S., White, S. D. M., Springel, V. +1 more·2007·Monthly Notices of the Royal Astronomical Society
DOI 10.1111/j.1365-2966.2007.12381.x
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Abstract

We use the Millennium Simulation (MS) to study the statistics of LCDM halo concentrations at z = 0. Our results confirm that the average halo concentration declines monotonically with mass; a power-law fits well the concentration-mass relation for over 3 decades in mass, up to the most massive objects to form in a LCDM universe (~ 10^15 h^-1 Msol). This is in clear disagreement with the predictions of the model proposed by Bullock et al. for these rare objects, and agrees better with the original predictions of Navarro, Frenk, & White. The large volume surveyed, together with the unprecedented numerical resolution of the MS, allow us to estimate with confidence the distribution of concentrations and, consequently, the abundance of systems with unusual properties. About one in a hundred cluster haloes (M200 >~ 3x10^14 h^-1 Msol) have concentrations exceeding c200 = 7.5, a result that may be used to interpret the likelihood of unusually strong massive gravitational lenses, such as Abell 1689, in the LCDM cosmogony. A similar fraction (1 in 100) of galaxy-sized haloes (M200 ~ 10^12 h^-1 Msol) have c200 < 4.5, an important constraint on models that attempt to reconcile the rotation curves of low surface-brightness galaxies by appealing to haloes of unexpectedly low concentration. We find that halo concentrations are independent of spin once haloes manifestly out of equilibrium are removed from the sample. Compared to their relaxed brethren, the concentrations of out-of-equilibrium haloes tend to be lower and to have more scatter, while their spins tend to be higher... (continue)

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Registry

Crossref · 10.1111/j.1365-2966.2007.12381.x

Cites

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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 fits to NFW profiles are limited to the radial range [0.05, 1] R_200.

    “As argued in previous studies (e.g. Neto et al. 2007; Schaller et al. 2015), we limit the fits to the radial range [0 . 05 , 1] R 200 .”

    From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Neto et al. 2007

    Section 2.5 (p. 6) says the authors adopted 0.05 < r/r_vir < 1 for their NFW fits. The Fig. 3 caption (p. 6) says those fits extend slightly beyond r_200, so the source supports the fitting range but not the claim that its boundary is R_200. (LLM, conf=0.91)

    Experimental — accuracy not yet measured

  • The ML concentration is equal to the median concentration of ∼1×10^12 M⊙ haloes.

    “The ML value for the concentration is, in fact, equal to the median concentration of ∼ 1 × 10 12 M ⊙ haloes (e.g. Neto et al. 2007; Hellwing et al. 2016)”

    From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Neto et al. 2007

    Section 3.1 (pp. 6–8) reports median concentration as a function of halo mass, including haloes near 10^12 h^-1 M⊙. It does not identify the citing paper’s ML concentration or establish that the two values are equal; its mass is also expressed in h^-1 M⊙ rather than M⊙. (LLM, conf=0.83)

    Experimental — accuracy not yet measured

  • Some haloes are not in equilibrium, typically because of transient events such as mergers; including such haloes would misrepresent the long-term relation between the DM distributions in the DMO and hydrodynamics simulations.

    “Some haloes are not in equilibrium, typically because of transient events such as mergers (e.g. see Neto et al. 2007); including such haloes would misrepresent the longterm relation between the DM distributions in the DMO and hydrodynamics simulations so we do not consider them further.”

    From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Neto et al. 2007

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Cites

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Research works printed but not linked: 2

  1. D'Onghia E., Navarro J. F., 2007, astro, arXiv:astro-ph/0703195 · arXiv
  2. Limousin M., et al., 2006, arXiv:astro-ph/0612165 · arXiv

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Authors
Neto, A. F., Gao, L., Bett, P., Cole, S., Navarro, J. F., Frenk, C. S., White, S. D. M., Springel, V., & Jenkins, A.
Affiliations
  • Universidade Federal do Rio Grande do Sul (BR)
  • Durham University (GB)
  • Max Planck Society (DE)
ORCID
Venue
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Published
2007-11-11
Volume
381
Issue
4
Pages
1450-1462
ISSN
  • 0035-8711 (ISSN-L)
  • 1365-2966
DOI
10.1111/j.1365-2966.2007.12381.x
OpenAlex
W1968752888
Cited by
764
References
52
Citations by year
2026: 5 · 2025: 17 · 2024: 20 · 2023: 23 · 2022: 34 · 2021: 38 · 2020: 41 · 2019: 32 · 2018: 37 · 2017: 38 · 2016: 55 · 2015: 58 · 2014: 43 · 2013: 57 · 2012: 68
FWCI
30.70
Type
journal article
Language
en
Open access
Locations
  • Monthly Notices of the Royal Astronomical Society (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • Durham Research Online (Durham University) (submittedVersion)
  • Max Planck Institute for Plasma Physics (submittedVersion)
  • Max Planck Digital Library (submittedVersion)
  • Durham Research Online (Durham University) (submittedVersion, cc-by)
  • MPG.PuRe (Max Planck Society) (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 › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
Keywords
dark matter halo concentration, concentration-mass relation, Millennium Simulation, LCDM cosmology, galaxy halos, gravitational lensing, Abell 1689, low surface brightness galaxies, halo spin

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