The DOI matches its Crossref record; 8 of the 8 references it cites were found in a registry or an index.
The Structure of Cold Dark Matter Halos
Open accessAbstract
We use N-body simulations to investigate the structure of dark halos in the standard cold dark matter cosmogony. Halos are excised from simulations of cosmologically representative regions and are resimulated individually at high resolution. We study objects with masses ranging from those of dwarf galaxy halos to those of rich galaxy clusters. The spherically averaged density profiles of all our halos can be fitted over two decades in radius by scaling a simple "universal" profile. The characteristic over- density of a halo, or equivalently its concentration, correlates strongly with halo mass in a way that reflects the mass dependence of the epoch of halo formation. Halo profiles are approximately isothermal over a large range in radii but are significantly shallower than r -2 near the center and steeper than r-2 near the virial radius. Matching the observed rotation curves of disk galaxies requires disk mass-to-light ratios to increase systematically with luminosity. Further, it suggests that the halos of bright galaxies depend only weakly on galaxy luminosity and have circular velocities significantly lower than the disk rotation speed. This may explain why luminosity and dynamics are uncorrelated in observed samples of binary galaxies and of satellite/spiral systems. For galaxy clusters, our halo models are consistent both with the presence of giant arcs and with the observed structure of the intracluster medium, and they suggest a simple explanation for the disparate estimates of cluster core radii found by previous authors. Our results also highlight two shortcomings of the CDM model. CDM halos are too concentrated to be consistent with the halo parameters inferred for dwarf irregulars, and the predicted abundance of galaxy halos is larger than the observed abundance of galaxies. The first problem may imply that the core structure of dwarf galaxies was altered by the galaxy formation process, and the second problem may imply that galaxies failed to form (or remain undetected) in many dark halos.
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Citations
Cites
Contraction of dark matter galactic halos due to baryonic infall
Blumenthal, G. R., Faber, S. M., Flores, R., & Primack, J. R. (1986) · The Astrophysical Journal · doi:10.1086/163867 · Cited by 1,213
Navarro, J. F., Frenk, C. S., & White, S. D. M. (1995) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/275.3.720 · Cited by 1,079
Self-citationThe formation of dark halos in a universe dominated by cold dark matter
Frenk, C. S., White, S. D. M., Davis, M., & Efstathiou, G. (1988) · The Astrophysical Journal · doi:10.1086/166213 · Cited by 541
Self-citationCold dark matter, the structure of galactic haloes and the origin of the Hubble sequence
Frenk, C. S., White, S. D. M., Efstathiou, G., & Davis, M. (1985) · Nature · doi:10.1038/317595a0 · Cited by 193
Self-citationThe massive halos of spiral galaxies
Zaritsky, D., & White, S. D. M. (1994) · The Astrophysical Journal · doi:10.1086/174840 · Cited by 155
Self-citationThe response of a spheroid to a disc field or were bulges ever ellipticals?
Barnes, J., & White, S. D. M. (1984) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/211.4.753 · Cited by 98
Self-citationPrimordial density fluctuations and the structure of galactic haloes
Quini, P. J., Salmon, J. K., & Zurek, W. H. (1986) · Nature · doi:10.1038/322329a0 · Cited by 79
Polarization of X-rays from Cygnus X-1: A test of the accretion disk model
Lightman, A., & Shapiro, S. (1976) · doi:10.1086/154131 · Cited by 25
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Research works printed but not linked: 4
- Blumenthal, G.R., Faber, S.M., Flores, R., & Primack, J.P. 1986, ApJ, 301, 27. Broeils, A.H. 1992a, Ph.D. Thesis, Gr oningen University.
- Navarro, J.F., Frenk, C.S., & White, S.D.M. 1995b, MNRAS, in press. Navarro, J.F., Eke, V.R., & Frenk, C.S. 1995, MN-
- Persic, M., & Salucci, P. 1991, ApJ, 368, 60. Persic, M., & Salucci, P. 1995, ApJS, in press. Persic, M., Salucci, P., & Stel, F. 1995, MNRAS, sub-
- Pierce, M., & Tully, B. 1988, ApJ, 330, 579. Press, W.H., & Schechter, P. 1974, ApJ, 187, 425.
Cited by
Sorted by citations
A Universal Density Profile from Hierarchical Clustering
Navarro, J. F., Frenk, C. S., & White, S. D. M. (1997) · The Astrophysical Journal · doi:10.1086/304888 · Cited by 9,917
“In Navarro et al. (1996) we discussed several of these in the context of the standard CDM cosmogony – rotation curves of giant and dwarf galaxies, satellite galaxy dynamics, hot gaseous atmospheres around galaxies and in clusters, strong and weak gravitational lensing – all provide interesting…”
BackgroundSelf-citationThe cosmological simulation code gadget-2
Springel, V. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.09655.x · Cited by 6,368
“…results based on simulation work is therefore quite long, including fundamental results such as the density profiles of dark matter halos (e.g. Navarro et al., 1996), the existence and dynamics of dark matter substructure (e.g. Tormen, 1997), the non-linear clustering properties of dark…”
BackgroundA Universal Density Profile from Hierarchical ClusteringPreprint
Navarro, J. F., Frenk, C. S., & White, S. D. M. (1996) · Cited by 6,275
Self-citationParticle dark matter: evidence, candidates and constraints
Bertone, G., Hooper, D., & Silk, J. (2005) · Physics Reports · doi:10.1016/j.physrep.2004.08.031 · Cited by 4,979
Modified gravity and cosmology
Clifton, T., Ferreira, P. G., Padilla, A., & Skordis, C. (2012) · Physics Reports · doi:10.1016/j.physrep.2012.01.001 · Cited by 4,630
Metadata
- Authors
- Navarro, J. F., Frenk, C. S., & White, S. D. M.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 1996-05
- Volume
- 462
- Pages
- 563
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W1532082951
- Cited by
- 8,544
- References
- 8
- Citations by year
- 2026: 312 · 2025: 481 · 2024: 483 · 2023: 436 · 2022: 431 · 2021: 436 · 2020: 412 · 2019: 391 · 2018: 436 · 2017: 356 · 2016: 400 · 2015: 367 · 2014: 327 · 2013: 295 · 2012: 332
- FWCI
- 72.71
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- Durham Research Online (Durham University) (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
- cold dark matter, dark matter halos, halo density profiles, isothermal halo, halo concentration, galaxy rotation curves, galaxy clusters, intracluster medium, giant arcs, dwarf irregular galaxies, galaxy formation, galaxy abundance
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