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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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de Blok, W. J. G. (2009) · Advances in Astronomy · doi:10.1155/2010/789293 · Cited by 934
“Here R200 is the radius at which the density contrast with respect to the critical density of the universe exceeds 200, roughlythe virial radius;V200 is the circular velocity atR200 (Navarro et al. 1996b).”
BackgroundMethodInfluentialMcMillan, P. J. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.18564.x · Cited by 789
PPPC 4 DM ID: a poor particle physicist cookbook for dark matter indirect detection
Cirelli, M., Corcella, G., Hektor, A., Hütsi, G., Kadastik, M., Paolo Panci, A., Raidal, M., Sala, F., & Strumia, A. (2011) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2011/03/051 · Cited by 988
Gómez, P., Nichol, R. C., Miller, C. J., Balogh, M. L., Goto, T., Zabludoff, A. I., Romer, A. K., Bernardi, M., Sheth, R. K., Hopkins, A., et al. (2003) · The Astrophysical Journal · doi:10.1086/345593 · Cited by 776
“In practice however, the region between Rv and Rt is not empty and a more realistic case is to assume that clusters or groups of galaxies follow, for example, the NFW mass density profile (Navarro et al. 1996).”
BackgroundDark Matter Annihilation at the Galactic Center
Paolo Gondolo, A., & Silk, J. I. (1999) · Physical Review Letters · doi:10.1103/physrevlett.83.1719 · Cited by 921
The statistics of CDM halo concentrations
Neto, A. F., Gao, L., Bett, P., Cole, S., Navarro, J. F., Frenk, C. S., White, S. D. M., Springel, V., & Jenkins, A. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.12381.x · Cited by 764
Self-citationXue, X.-X., Rix, H., Zhao, G., Fiorentin, P. R., Naab, T., Steinmetz, M., van den Bosch, F. C., Beers, T. C., Lee, Y. S., Bell, E. F., et al. (2008) · The Astrophysical Journal · doi:10.1086/589500 · Cited by 716
“In turn, the extended stellar distributions of galaxies, in particular the stellar halos of nearby galaxies, offer some of the best probes to test generic predictions about the nature of dark matter mass profiles (Navarro et al. 1996).”
BackgroundMethodCappellari, M., Scott, N., Alatalo, K., Blitz, L., Bois, M., Bournaud, F., Bureau, M., Crocker, A., Davies, R. L., Davis, T. A., et al. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt562 · Cited by 746
“We then adopt the halo mass–concentration M200−c200 relation (Navarro et al. 1996) as given by Klypin, Trujillo-Gomez & Primack (2011) to make the halo profile a unique function of its mass M200.”
MethodModified Newtonian Dynamics as an Alternative to Dark Matter
Sanders, R. H., & McGaugh, S. S. (2002) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.40.060401.093923 · Cited by 728
“…high precision and resolution, this hypothesis has gained predictive power on the scale of galaxies– a power that considerably restricts the freedom to arrange dark matter as one would wish in order to explain the form and magnitude of the discrepancy in any particular system (Navarro et al. 1996).”
BackgroundMandelbaum, R., Seljak, U., Kauffmann, G., Hirata, C. M., & Brinkmann, J. (2006) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.10156.x · Cited by 728
“The DM profiles are assumed here to be NFW profiles (Navarro et al. 1996) with concentration parameter (Bullock et al. 2001; Eke et al. 2001) cdm = 10 ( Mcent Mnl(z) )−0.13 (5) where Mnl(z), the nonlinear mass scale, is defined such that the rms linear density fluctuation extrapolated to redshift z…”
BackgroundInfluentialCappellari, M., McDermid, R. M., Alatalo, K., Blitz, L., Bois, M., Bournaud, F., Bureau, M., Crocker, A., Davies, R. L., Davis, T. A., et al. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt644 · Cited by 695
Powerful Outflows and Feedback from Active Galactic Nuclei
King, A. R., & Pounds, K. (2015) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-082214-122316 · Cited by 813
“McQuillin & McLaughlin (2012) show this explicitly for three widely–used density distributions (Hernquist 1990; Navarro et al. 1996, 1997; and Dehnen &McLaughlin 2005): the results are in practice scarcely distinguishable from (42).”
BackgroundΛCDM‐based Models for the Milky Way and M31. I. Dynamical Models
Klypin, A. A., Zhao, H., & Somerville, R. S. (2002) · The Astrophysical Journal · doi:10.1086/340656 · Cited by 692
How supernova feedback turns dark matter cusps into coresPreprint
Pontzen, A., & Governato, F. (2012) · Cited by 756
Bœhm, C., & Fayet, P. (2004) · Nuclear Physics B · doi:10.1016/j.nuclphysb.2004.01.015 · Cited by 675
A UNIVERSAL MASS PROFILE FOR DWARF SPHEROIDAL GALAXIES?
Walker, M. G., Mateo, M. L., Olszewski, E. W., Peñarrubia, J., Evans, N. W., & Gilmore, G. F. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/704/2/1274 · Cited by 680
Adaptive Refinement Tree: A New High‐Resolution N ‐Body Code for Cosmological Simulations
Kravtsov, A. V., Klypin, A. A., & Khokhlov, A. M. (1997) · The Astrophysical Journal Supplement Series · doi:10.1086/313015 · Cited by 692
“20) presented by Navarro et al. (1996a) and have cuspy ( ρ ( r ) ∝ r − 1 ) structure in the central ( r < 10 h − 1 kpc) parts of a halo with no indications of a core down to the resolution limit of our simulations.”
BackgroundThe subhalo populations of ΛCDM dark haloes
Gao, L., White, S. D. M., Jenkins, A. R., Stoehr, F., & Springel, V. (2004) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2004.08360.x · Cited by 657
Self-citationHow Many Galaxies Fit in a Halo? Constraints on Galaxy Formation Efficiency from Spatial Clustering
Scoccimarro, R., Sheth, R. K., Hui, L., & Jain, B. (2001) · The Astrophysical Journal · doi:10.1086/318261 · Cited by 659
A METHOD FOR MEASURING (SLOPES OF) THE MASS PROFILES OF DWARF SPHEROIDAL GALAXIES
Walker, M. G., & Peñarrubia, J. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/742/1/20 · Cited by 712
“…of Cambridge, Madingley Road, Cambridge CB30HA 3 Hubble Fellow volving baryons might alter the original structure of a dark matter halo (e.g., Blumenthal et al. 1986; Navarro et al. 1996; El-Zant et al. 2001; Gnedin et al. 2004; Tonini et al. 2006; Governato et al. 2010; Pontzen & Governato 2011).”
BackgroundOrigin and propagation of extremely high-energy cosmic rays
Bhattacharjee, P., & Günter Sigl, A. (2000) · Physics Reports · doi:10.1016/s0370-1573(99)00101-5 · Cited by 646
Schaye, J., & Vecchia, C. D. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.12639.x · Cited by 650
Clowe, D., Gonzalez, A., & Markevitch, M. (2004) · The Astrophysical Journal · doi:10.1086/381970 · Cited by 638
“We tried fitting a singular isothermal sphere, a NFW model (Navarro et al. 1996), and a King model to the data and found that the King model was marginally preferred over the NFW model, as measured by the δχ2 between the model reduced shear profile and the data.”
MethodGovernato, F., Zolotov, A., Pontzen, A., Christensen, C., Oh, S.-H., Brooks, A. M., Quinn, T., Shen, S., & Wadsley, J. W. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.20696.x · Cited by 652
“DM-only simulations predict that DM halos should follow a quasi– universal Einasto profile (Navarro et al. 1996b; Moore et al. 1999; Reed et al. 2005; Macciò et al. 2009; Stadel et al. 2009; Navarro et al. 2010), defined by a power law density profile ρ ∝ rα with −1.5 < α < −1 in their central…”
BackgroundInfluentialMilosavljević, M., & Merritt, D. (2001) · The Astrophysical Journal · doi:10.1086/323830 · Cited by 663
The RAVE survey: constraining the local Galactic escape speed
Smith, M. C., Ruchti, G. R., Helmi, A., Wyse, R. F. Ġ., Fulbright, J. P., Freeman, K. C., Navarro, J. F., Seabroke, G. M., Steinmetz, M., Williams, M., et al. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.11964.x · Cited by 629
“For this model we revert to our original Miyamoto & Nagai (1975) disc, as used for the uncontracted NFW profile.”
BackgroundInfluentialSelf-citationHelmi, A., van Leeuwen, F., McMillan, P. J., Massari, D., Antoja, T., Robin, A. C., Lindegren, L., Bastian, U., Arenou, F., Babusiaux, C., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201832698 · Cited by 648
High-resolution rotation curves of low surface brightness galaxies
de Blok, W. J. G., & Bosma, A. (2002) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20020080 · Cited by 617
“The NFW mass density distribution (Navarro et al. 1996, 1997) takes the form ρNFW (R) = ρi (R/Rs) (1 +R/Rs) 2 (4) where Rs is the characteristic radius of the halo and ρi is related to the density of the universe at the time of collapse.”
BackgroundCosmological simulations of galaxy formation
Vogelsberger, M., Marinacci, F., Torrey, P., & Puchwein, E. (2020) · Nature Reviews Physics · doi:10.1038/s42254-019-0127-2 · Cited by 710
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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