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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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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
Flagged first, then by citations
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
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Environmental influences on dark matter haloes and consequences for the galaxies within them
Lemson, G., & Kauffmann, G. (1999) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.1999.02090.x · Cited by 233
The Frontier Fields lens modelling comparison project
Meneghetti, M., Natarajan, P., Coe, D., Contini, E., Lucia, G. D., Giocoli, C., Acebrón, A., Borgani, S., Bradač, M., Diego, J. M., et al. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx2064 · Cited by 251
“We can choose either an elliptical Navarro et al. (1996) profile (eNFW), or, also PIEMD for the cluster’s dark matter halo.”
MethodUpdated Nearby Galaxy Catalog.Preprint
Karachentsev, I. D., Makarov, D. I., & Kaisina, E. I. (2016) · Cited by 231
LoCuSS: Subaru Weak Lensing Study of 30 Galaxy Clusters
Okabe, N., Takada, M., Umetsu, K., Futamase, T., & Smith, G. P. (2010) · University of Birmingham Research Portal (University of Birmingham) · Cited by 229
Dark Matter and Collider Phenomenology of Universal Extra DimensionsPreprint
Hooper, D., & Profumo, S. (2007) · Cited by 232
The Many Manifestations of Downsizing: Hierarchical Galaxy Formation Models confront Observations.Preprint
Fontanot, F., Lucia, G. D., Monaco, P., Somerville, R. S., & Santini, P. (2009) · Cited by 227
Laporte, C. F. P., Johnston, K. V., Gómez, F. A., Garavito-Camargo, N., & Besla, G. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1574 · Cited by 230
THE NUCLEUS OF THE SAGITTARIUS DSPH GALAXY AND M54: A WINDOW ON THE PROCESS OF GALAXY NUCLEATION
Bellazzini, M., Ibata, R., Chapman, S. C., Mackey, D., Monaco, L., Irwin, M. J., Martin, N. F., Lewis, G. F., & Dalessandro, E. (2008) · The Astronomical Journal · doi:10.1088/0004-6256/136/3/1147 · Cited by 229
Simulating observations of dark matter dominated galaxies: towards the optimal halo profile
de Blok, W. J. G., Bosma, A., & McGaugh, S. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2003.06330.x · Cited by 232
Gravitational clustering of relic neutrinos and implications for their detection
Ringwald, A., & Wong, Y. Y. Y. (2004) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2004/12/005 · Cited by 251
Morphological evolution of discs in clusters
Mastropietro, C., Moore, B., Mayer, L., Debattista, V. P., Piffaretti, R., & Stadel, J. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.09579.x · Cited by 236
The next-generation liquid-scintillator neutrino observatory LENA
Wurm, M. C., Beacom, J. F., Bezrukov, L. B., et al. (2012) · Astroparticle Physics · doi:10.1016/j.astropartphys.2012.02.011 · Cited by 228
A review of the discovery reach of directional Dark Matter detection
Mayet, F., Green, A. M., Battat, J., Billard, J., Bozorgnia, N., Gelmini, G. B., Paolo Gondolo, A., Kavanagh, B. J., Lee, S. K., Loomba, D., et al. (2016) · Physics Reports · doi:10.1016/j.physrep.2016.02.007 · Cited by 228
Dark matter and visible baryons in M33
Corbelli, E. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2003.06531.x · Cited by 214
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Fan, J., & Matthew Reece, B. (2013) · Journal of High Energy Physics · doi:10.1007/jhep10(2013)124 · Cited by 254
Gamma ray signals from dark matter: Concepts, status and prospects
Bringmann, T., & Weniger, C. (2012) · Physics of the Dark Universe · doi:10.1016/j.dark.2012.10.005 · Cited by 228
“The commonly used Navarro-Frenk-White (NFW) profile [74], for example, is obtained for (α, β, γ) = (1, 3, 1) (with rs ≃ 20 kpc in case of the Milky Way); the cored isothermal profile follows when setting (α, β, γ) = (2, 2, 0) and rs ≃ 3.”
MethodClusters of galaxies with modified Newtonian dynamics
Sanders, R. H. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2003.06596.x · Cited by 244
Black holes in galaxies: Environmental impact on gravitational-wave generation and propagation
Cardoso, V., Destounis, K., Duque, F., et al. (2022) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.105.l061501 · Cited by 226
Structure of Dark Matter Halos from Hierarchical Clustering
Fukushige, T., & Makino, J. (2001) · The Astrophysical Journal · doi:10.1086/321666 · Cited by 212
Auger, M. W., Treu, T., Gavazzi, R., Bolton, A. S., Koopmans, L. V. E., & Marshall, P. J. (2010) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/721/2/l163 · Cited by 224
“Numerical simulations of cold dark matter (CDM) halos predict density distributions with an inner logarithmic slope dlnρ/dlnr = −1 and a slope of dlnρ/dlnr = −3 at large radii (Navarro et al. 1996, 2010, hereafter NFW).”
BackgroundSánchez-Conde, M. Á., & Prada, F. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1014 · Cited by 225
Taylor, J. E., & Babul, A. (2001) · The Astrophysical Journal · doi:10.1086/322276 · Cited by 226
“In figure 9, the solid curves are for VW S1 as before, the long-dashed curves are for the satellite model used by WMH, and the dot-dashed curves are for a satellite with an NFW profile (Navarro et al. 1996, 1997) of comparable concentration.”
MethodThe Local Group on FIRE: dwarf galaxy populations across a suite of hydrodynamic simulations
Garrison-Kimmel, S., Hopkins, P. F., Wetzel, A. R., Bullock, J. S., Boylan-Kolchin, M., Kereš, D., Faucher‐Giguère, C., El-Badry, K., Lamberts, A., Quataert, E., et al. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1317 · Cited by 242
Baryonic solutions and challenges for cosmological models of dwarf galaxies
Sales, L. V., Wetzel, A. R., & Fattahi, A. (2022) · Nature Astronomy · doi:10.1038/s41550-022-01689-w · Cited by 308
Dark Matter and the First Stars: A New Phase of Stellar Evolution
Spolyar, D., Freese, K., & Paolo Gondolo, A. (2008) · Physical Review Letters · doi:10.1103/physrevlett.100.051101 · Cited by 223
A halo mass—concentration relation from weak lensing
Mandelbaum, R., Seljak, U., & Hirata, C. M. (2008) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2008/08/006 · Cited by 221
Statistics of Physical Properties of Dark Matter Clusters
Shaw, L. D., Weller, J., Ostriker, J. P., & Bode, P. W. (2006) · The Astrophysical Journal · doi:10.1086/505016 · Cited by 216
“…numerical precision—thus allowing the accurate identification of low-mass subhalos and measurement of the properties in the innermost regions—many previous studies have adopted a resimulation technique (e.g., Navarro et al. 1995, 1996, 2004; Gao et al. 2005; Moore et al. 1999; Reed et al. 2005a).”
MethodSearching for cool core clusters at high redshift
Santos, J. S., Rosati, P., Tozzi, P., Böhringer, H., Ettori, S., & Bignamini, A. (2008) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20078815 · Cited by 228
Splashback in accreting dark matter halos
Adhikari, S., Dalal, N., & Chamberlain, R. T. (2014) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2014/11/019 · Cited by 246
An over-massive black hole in the compact lenticular galaxy NGC 1277
van den Bosch, R. C. E., Gebhardt, K., Gültekin, K., van de Ven, G., van der Wel, A., & Walsh, J. L. (2012) · Nature · doi:10.1038/nature11592 · Cited by 220
A constant dark matter halo surface density in galaxiesPreprint
Donato, F., Gentile, G., Salucci, P., Martins, C. F., Wilkinson, M. I., Gilmore, G. F., Grebel, E. K., Koch, A., & Wyse, R. F. Ġ. (2009) · Cited by 218
Constraints on star formation driven galaxy winds from the mass-metallicity relation at z= 0
Peeples, M. S., & Shankar, F. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.19456.x · Cited by 221
Duffy, A. R., Schaye, J., Kay, S. T., Dalla Vecchia, C., Battye, R. A., & Booth, C. M. (2010) · MPG.PuRe (Max Planck Society) · Cited by 220
There's no place like home? Statistics of Milky Way-mass dark matter haloes
Boylan-Kolchin, M., Springel, V., White, S. D. M., & Jenkins, A. R. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16774.x · Cited by 228
“While numerical simulations have shown that dark matter halos have a nearly universal density profile (Navarro et al. 1996, 1997, hereafter NFW), the radial scale of the profile does not follow the virial scaling of R ∝ M1/3vir .”
BackgroundSelf-citationRadiative natural supersymmetry: Reconciling electroweak fine-tuning and the Higgs boson mass
Baer, H., Barger, V. D., Huang, P., et al. (2013) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.87.115028 · Cited by 220
Cusps in cold dark matter haloes
Diemand, J., Zemp, M., Moore, B., et al. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.09601.x · Cited by 219
How Lumpy Is the Milky Way’s Dark Matter Halo?
Johnston, K. V., Spergel, D. N., & Haydn, C. (2002) · The Astrophysical Journal · doi:10.1086/339791 · Cited by 227
NGC 3741: the dark halo profile from the most extended rotation curve
Gentile, G., Salucci, P., Klein, U., & Granato, G. L. (2006) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.11283.x · Cited by 218
Maximal Disks and the Tully‐Fisher Relation
Courteau, S., & Rix, H. (1999) · The Astrophysical Journal · doi:10.1086/306872 · Cited by 218
H I KINEMATICS AND DYNAMICS OF MESSIER 31
Chemin, L., Claude Carignan, A., & Foster, T. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/705/2/1395 · Cited by 221
HydrodynamicalN-body simulations of coupled dark energy cosmologies
Baldi, M., Pettorino, V., Robbers, G., & Springel, V. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15987.x · Cited by 225
Energetic galaxy-wide outflows in high-redshift ultraluminous infrared galaxies hosting AGN activity
Harrison, C. M., Alexander, D. M., Swinbank, A. M., Smail, I. R., Alaghband-Zadeh, S., Bauer, F. E., Chapman, S. C., Moro, A. D., Hickox, R. C., Ivison, R. J., et al. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21723.x · Cited by 215
“Assuming a static dark matter halo with a mass of≈1013 M⊙ (expected for these sources; Hickox et al. 2012), a Navarro Frenk and White (NFW; Navarro et al. 1996) density profile, and a point mass of≈1011 M⊙ (i.e., the host galaxy), a particle initially at ≈4 kpc from the centre of the host galaxy…”
BackgroundUniversal gas density and temperature profile
Komatsu, E., & Seljak, U. (2001) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2001.04838.x · Cited by 224
“Often it is close to the value where the slope isα = 2 (Navarro et al. 1996, 1997; Moore et al. 1998).”
BackgroundSalucci, P., Lapi, A., Tonini, C., et al. (2007) · Cited by 218
Measures of galaxy environment - I. What is ‘environment’?
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Mass and shape of the Milky Way’s dark matter halo with globular clusters from Gaia and Hubble
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Astrophysics with the Spatially and Spectrally Resolved Sunyaev-Zeldovich Effects
Mroczkowski, T. K., Nagai, D., Basu, K., Chluba, J., Sayers, J., Adam, R., Churazov, E., Crites, A. T., Mascolo, L. D., Eckert, D., et al. (2019) · Space Science Reviews · doi:10.1007/s11214-019-0581-2 · Cited by 218
ON THE SHOULDERS OF GIANTS: PROPERTIES OF THE STELLAR HALO AND THE MILKY WAY MASS DISTRIBUTION
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“We essentially construct a model of the Galactic potential with three components: an oblate spheroidal bulge, an axisymmetric disk described by Miyamoto & Nagai (1975) and a spherical dark halo described by aΛCDM motivated Navarro-Frank-White (NFW, Navarro et al. 1996) profile.”
MethodOn the life and death of satellite haloes
Taffoni, G., Mayer, L., Colpi, M., & Governato, F. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2003.06395.x · Cited by 206
“Here, we use the so called ‘universal density profile’ of Navarro et al. (1996): ρ(r ) = Mh 4πR3h δc (chx)(1 + chx)2 , (1) where x = r/Rh is the dimensionless radius in units of the virial radius Rh, Mh is the mass of the halo inside Rh, ch = r s/Rh is the concentration parameter (r s is a scale…”
MethodCLASH: THE CONCENTRATION-MASS RELATION OF GALAXY CLUSTERS
Merten, J., Meneghetti, M., Postman, M., Umetsu, K., Zitrin, A., Medezinski, E., Nonino, M., Koekemoer, A. M., Melchior, P., Gruen, D., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/806/1/4 · Cited by 237
“As shown by numerical simulations (Navarro et al. 1996), dark matter tends to arrange itself following a specific, spherically symmetric density profile ρNFW(r) = ρs r/rs (1 + r/rs) 2 , (1) where the only two parameters ρs and rs are a scale density and a scale radius.”
BackgroundHALO OCCUPATION DISTRIBUTION MODELING OF CLUSTERING OF LUMINOUS RED GALAXIES
Zheng, Z., Zehavi, I., Eisenstein, D. J., Weinberg, D. H., & Jing, Y. P. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/707/1/554 · Cited by 225
“The distribution profile of L∗ satellite galaxies inside halos is assumed to follow the Navarro–Frenk–White (NFW) profile (Navarro et al. 1995, 1996, 1997) with a concentration parameter c = c0(M/Mnl)β , where Mnl ∼ 1.5 × 1012 h−1 M is the nonlinear mass at z ∼ 0.3 and β is fixed to −0.13 (Bullock…”
BackgroundInfluentialÁvila-Reese, V., Firmani, C., & Hernández, X. (1998) · The Astrophysical Journal · doi:10.1086/306136 · Cited by 207
The apostle project: Local Group kinematic mass constraints and simulation candidate selection
Fattahi, A., Navarro, J. F., Sawala, T., Frenk, C. S., Oman, K. A., Crain, R. A., Furlong, M., Schaller, M., Schaye, J., Theuns, T., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2970 · Cited by 214
Self-citationDark matter cores and cusps: the case of multiple stellar populations in dwarf spheroidals
Amorisco, N. C., & Evans, N. W. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.19684.x · Cited by 213
“In particular, the prediction of a cusped density profile for dark matter haloes (Navarro et al. 1996) has naturally focused attention on the structure of the innermost parts.”
BackgroundThe rotation curves shapes of late-type dwarf galaxies
Swaters, R. A., Sancisi, R., van Albada, T. S., & van der Hulst, J. M. (2008) · Astronomy and Astrophysics · doi:10.1051/0004-6361:200810516 · Cited by 213
“…focused on the shape of the rotation curve in the central regions of these galaxies, because these inner rotation curve shapes provide a powerful test of models of galaxy formation in a cold dark matter dominated universe (e.g., Navarro et al. 1996, 1997; Bullock et al. 2001; Power et al. 2003).”
BackgroundGas Stripping of Dwarf Galaxies in Clusters of Galaxies
Mori, M., & Burkert, A. M. (2000) · The Astrophysical Journal · doi:10.1086/309140 · Cited by 213
More Satellites of Spiral Galaxies
Zaritsky, D., Smith, R., Frenk, C. S., et al. (1997) · The Astrophysical Journal · doi:10.1086/303784 · Cited by 213
“Given the recent results from simulations on the behavior of disks and halos, the lack of a strong signal is not as surprising as it once was and may be consistent with the parameterization of halo rotation curves found by Navarro et al. (1996).”
ResultSelf-citationX‐Ray Gas Density Profile of Clusters of Galaxies from the Universal Dark Matter Halo
Makino, N., Sasaki, S., & Suto, Y. (1998) · The Astrophysical Journal · doi:10.1086/305507 · Cited by 203
Tidal tailspin cold dark matter cosmologies
Springel, V., & White, S. D. M. (1999) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.1999.02613.x · Cited by 214
Self-citationGrowth and activity of black holes in galaxy mergers with varying mass ratios
Capelo, P. R., Volonteri, M., Dotti, M., et al. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu2500 · Cited by 211
Diffuse gamma ray constraints on annihilating or decaying Dark Matter after Fermi
Cirelli, M., Panci, P., & Serpico, P. D. (2010) · Nuclear Physics B · doi:10.1016/j.nuclphysb.2010.07.010 · Cited by 211
Dolag, K., Komatsu, E., & Sunyaev, R. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2035 · Cited by 226
“We convert M to M200m using an NFW profile (Navarro et al. 1996, 1997) with the concentration parameter of Duffy et al. (2008) (see, e.g., Eq.”
MethodCosmology with a stiff matter era
Chavanis, P.-H. (2015) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.92.103004 · Cited by 211
Dynamical Blueprints for Galaxies
Widrow, L. M., Pym, B., & Dubinski, J. (2008) · The Astrophysical Journal · doi:10.1086/587636 · Cited by 216
“The latter was constructed to yield the so-called NFW profile (Navarro et al. 1996) NFW(r) ¼ h r=ahð Þ 1þ r=ahð Þ2 : ð4Þ Widrow & Dubinski (2005) altered these DFs in an attempt to account for the gravitational potential of the other components, although the modifications were somewhat ad hoc.”
BackgroundMethodGhirardini, V., Eckert, D., Ettori, S., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833325 · Cited by 210
“For the present work, we adopt as our reference mass model the backward NFW results, which were obtained by assuming that the mass profile follows a Navarro-Frenk-White shape (Navarro et al. 1996) with scale radius and concentration c200 as free parameters.”
MethodGamma Ray Signals from Dark Matter: Concepts, Status and ProspectsPreprint
Bringmann, T., & Weniger, C. (2016) · Cited by 207
Making the Case for Conformal GravityPreprint
Mannheim, P. D. (2011) · Cited by 244
Wong, K. C., Suyu, S. H., Auger, M. W., Bonvin, V., Courbin, F., Fassnacht, C. D., Halkola, A., Rusu, C. E., Sluse, D., Sonnenfeld, A., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw3077 · Cited by 207
“Composite Model Parameters Parameter Marginalized Constraints Composite Composite,AGNmask+1 Composite,Arcmask+1,50src Stellar M/L (M⊙/L⊙)a 2.5 +0.1 −0.1 2.6 +0.2 −0.2 2.3 +0.1 −0.1 NFW κ0,h 0.41 +0.03 −0.03 0.36 +0.03 −0.03 0.39 +0.01 −0.01 NFW rs (′′) 8.43 +0.58 −1.94 9.43 +0.69 −0.94 8.96 +0.28 −0.26 NFW q 0.82+0.01…”
InfluentialNishimichi, T., Takada, M., Takahashi, R., Osato, K., Shirasaki, M., Oogi, T., Miyatake, H., Oguri, M., Murata, R., Kobayashi, Y., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab3719 · Cited by 213
“Properties and cosmological dependences of the mass density profiles around halos have been extensively studied (e.g., Navarro et al. 1996).”
BackgroundHot Gas In and Around Elliptical Galaxies
Mathews, W. G., & Brighenti, F. (2003) · CERN Document Server (European Organization for Nuclear Research) · Cited by 208
Galaxy threshing and the origin of ultra-compact dwarf galaxies in the Fornax cluster
Bekki, K., Couch, W. J., Drinkwater, M. J., et al. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2003.06916.x · Cited by 208
Small-scale clumps in the galactic halo and dark matter annihilation
Berezinsky, V. S., Dokuchaev, V. I., & Eroshenko, Y. N. (2003) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.68.103003 · Cited by 207
Simulations of Cosmic Chemical Enrichment
Kobayashi, C., Springel, V., & White, S. D. M. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.11555.x · Cited by 207
Self-citationThe mass profile and accretion history of cold dark matter haloes
Ludlow, A. D., Navarro, J. F., Boylan-Kolchin, M., Bett, P. E., Angulo, R. E., Li, M., White, S. D. M., Frenk, C. S., & Springel, V. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt526 · Cited by 217
Self-citationPhase-space Analysis in the Group and Cluster Environment: Time Since Infall and Tidal Mass Loss
Rhee, J., Smith, R., Choi, H., Yi, S. K., Jaffé, Y. L., Candlish, G., & Sánchez-Janssen, R. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa6d6c · Cited by 212
IMPACT OF CLUSTER PHYSICS ON THE SUNYAEV-ZEL'DOVICH POWER SPECTRUM
Shaw, L. D., Nagai, D., Bhattacharya, S., & Lau, E. T. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/725/2/1452 · Cited by 236
“Dark matter halo properties are determined by a Navarro-Frenk-White (NFW) density profile (Navarro et al. 1996, 1997) of the form, ρDM (r) = ρs x(1 + x)2 , (5) where x ≡ r/rs, rs is the NFW scale radius, and ρs is a normalization constant.”
BackgroundScannapieco, C., Tissera, P. B., White, S. D. M., & Springel, V. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.09574.x · Cited by 207
Self-citationUnderstanding the shape and diversity of dwarf galaxy rotation curves in ΛCDM
Read, J. I., Iorio, G., Agertz, O., & Fraternali, F. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1876 · Cited by 215
“G A ] 1991; Moore 1994; Navarro et al. 1996b) in stark contrast with observed rotation curves that favour constant density ‘cores’ (e.g. Flores & Primack 1994; de Blok et al. 2001; de Blok 2009; Oh et al. 2011, 2015; Hague & Wilkinson 2013, 2014; Adams et al. 2014; Oh et al. 2015).”
BackgroundMethodResultInfluentialA Test of the Collisional Dark Matter Hypothesis from Cluster Lensing
Miralda‐Escudé, J. (2002) · The Astrophysical Journal · doi:10.1086/324138 · Cited by 243
The SPTpol Extended Cluster Survey
Bleem, L., Bocquet, S., Stalder, B., Gladders, M., Ade, P., Allen, S., Anderson, A., Annis, J., Ashby, M., Austermann, J., et al. (2019) · Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ab6993 · Cited by 136
“We convert M c500 to M200 m assuming a Navarro, Frenk, and White (Navarro et al. 1996) profile and the concentration–mass relation from Child et al. (2018).99 We invert our relation as òl l”
MethodConstraining the Galaxy's dark halo with RAVE stars
Piffl, T., Binney, J. J., McMillan, P. J., Steinmetz, M., Helmi, A., Wyse, R. F. Ġ., Bienaymé, O., Bland‐Hawthorn, J., Freeman, K. C., Gibson, B. K., et al. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1948 · Cited by 198
Self-citationGalactic accretion and the outer structure of galaxies in the CDM model
Cooper, A. P., D’Souza, R., Kauffmann, G., Wang, J., Boylan-Kolchin, M., Guo, Q., Frenk, C. S., & White, S. D. M. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt1245 · Cited by 198
Self-citationCôté, S., Claude Carignan, A., & Freeman, K. C. (2000) · The Astronomical Journal · doi:10.1086/316883 · Cited by 192
“These dwarf rotation curves are also difficult to Ðt with the CDM model curves of Navarro et al. (1996a) which are too concentrated.”
BackgroundBekki, K. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15431.x · Cited by 202
(In)direct detection of boosted dark matter
Agashe, K., Yanou Cui, A., Necib, L., et al. (2014) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2014/10/062 · Cited by 202
The Phoenix Project: the dark side of rich Galaxy clusters
Gao, L., Navarro, J. F., Frenk, C. S., Jenkins, A., Springel, V., & White, S. D. M. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21564.x · Cited by 203
“The thin dashed lines in Fig.4 indicate the best-fit NFW (brown) and Einasto (magenta) profiles, computed as describd in the Appendix.”
BackgroundMethodInfluentialSelf-citationA universal density slope – Velocity anisotropy relation for relaxed structures
Hansen, S. H., & Moore, B. (2005) · New Astronomy · doi:10.1016/j.newast.2005.09.001 · Cited by 207
THE LUMINOSITY PROFILE AND STRUCTURAL PARAMETERS OF THE ANDROMEDA GALAXY
Courteau, S., Widrow, L. M., McDonald, M., Guhathakurta, P., Gilbert, K. M., Zhu, Y., Beaton, R. L., & Majewski, S. R. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/739/1/20 · Cited by 199
“Note that at large radii, the Hernquist model (Hernquist 1990) and the Navarro–Frenk–White (NFW) function (Navarro et al. 1996), as explored for the M31 halo by, e.g., Ibata et al. (2007) and Tanaka et al. (2010), are special cases of our power-law model.”
MethodGravitational lensing of wormholes in the galactic halo region
Kuhfittig, P. K. F. (2014) · The European Physical Journal C · doi:10.1140/epjc/s10052-014-2818-2 · Cited by 201
Observational evidence for primordial black holes: A positivist perspective
Carr, B. J., Clesse, S., García-Bellido, J., Hawkins, M. R. S., & Kühnel, F. (2024) · Physics Reports · doi:10.1016/j.physrep.2023.11.005 · Cited by 256
The Origin of the Brightest Cluster GalaxiesPreprint
Dubinski, J., & Labs, M. (1997) · Cited by 198
Possible existence of wormholes in the galactic halo region
Farook Rahaman, A., Kuhfittig, P. K. F., Ray, S., & Islam, N. (2014) · The European Physical Journal C · doi:10.1140/epjc/s10052-014-2750-5 · Cited by 212
DWARF GALAXY ANNIHILATION AND DECAY EMISSION PROFILES FOR DARK MATTER EXPERIMENTS
Geringer-Sameth, A., Koushiappas, S. M., & Walker, M. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/801/2/74 · Cited by 261
“In addition, the density of the inner parts of a halo is also roughly set at the time of formation, following a distribution in concentration, c ≡ Rvir/rs, where Rvir is the radius of the virialized region (Navarro et al. 1996).”
BackgroundMethodThe hidden giant: discovery of an enormous Galactic dwarf satellite in Gaia DR2
Torrealba, G., Belokurov, V. A., Koposov, S. E., Li, T. S., Walker, M. G., Sanders, J. L., Geringer-Sameth, A., Zucker, D. B., Kuehn, K. W., Evans, N. W., et al. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1624 · Cited by 220
“…context, we first consider the properties of dark matter haloes that might host Ant 2 while following the NFW enclosed-mass profile that characterizes haloes formed in N-body simulations (Navarro et al. 1996b; Navarro, Frenk & White 1997): MNFW(r) = 4πr3s ρs [ ln ( 1 + r rs ) − r/rs 1 + r/rs ] .”
BackgroundDark matter and cosmic structure
Frenk, C., & White, S. D. M. (2012) · MPG.PuRe (Max Planck Society) · Cited by 198
Self-citationCOOLING, AGN FEEDBACK, AND STAR FORMATION IN SIMULATED COOL-CORE GALAXY CLUSTERS
Li, Y., Bryan, G. L., Ruszkowski, M., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/811/2/73 · Cited by 199
“This allows us to fit an NFW profile (Navarro et al. 1996) to the dark matter halo: ρ(r) = ρ0 r Rs (1 + rRs ) 2 , (5) where ρ0 is found to be 8.42×10−26 g cm−3, and the scale radius Rs = 351.7 kpc.”
MethodInfluentialCosmic ray feedback in hydrodynamical simulations of galaxy formation
Jubelgas, M., Springel, V., Enßlin, T. A., & Pfrommer, C. (2007) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20065295 · Cited by 197
Mamon, G. A., Biviano, A., & Boué, G. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sts565 · Cited by 209
“(Burkert) (36) The NFW model has long been known to fit well the density profiles ofΛCDM haloes (Navarro et al. 1996), and while Navarro et al. (2004) found that Einasto models fit them even better, MBM10 found that the NFW model describes the outer LOS velocity dispersion profile of the DM…”
BackgroundDetermination of dark matter properties at high-energy colliders
Baltz, E. A., Marco Battaglia, A., Peskin, M. E., & Wizansky, T. (2006) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.74.103521 · Cited by 199
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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