The Density Profiles of the Dark Matter Halo Are Not Universal

Jing, Y. P.; Suto, Yasushi

doi:10.1086/312463

Cited by 391 publications

(482 citation statements)

References 24 publications

Supporting

Mentioning

437

Contrasting

Unclassified

Order By: Relevance

“…In the outer region, the density proÐles are very similar for all runs. The dependence of the power-law index of the inner cusp on halo mass observed by Jing & Suto (2000) was not reproduced in our simulations. In the following subsections we discuss the self-similar growth of the halo (°3.4), the universality of the proÐle (°3.5), and the mechanism for selfsimilar growth (°3.6).…”

Section: Other Numerical E †Ectscontrasting

confidence: 58%

“…Moore et al (1998Moore et al ( , 1999 and Ghigna et al (2000) performed simulations with up to 4 ] 106 particles and obtained results similar to ours. They found that cluster-sized halos also have steeper cusps than those in the NFW proÐle, and they proposed a modiÐed universal proÐle : o \ o 0 /M(r/r s )1.5 ] On the other hand, Jing & Suto (2000) [1 ] (r/r s )1.5]N. found that the density proÐle of dark matter is not universal. They performed a series of N-body simulations and concluded that the power of the cusp depends on mass.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Structure of Dark Matter Halos from Hierarchical Clustering

Fukushige

Makino

2001

ApJ

201

189

View full text Add to dashboard Cite

We investigate the structure of the dark matter halo formed in the cold dark matter scenario using N-body simulations. We simulated 12 halos with masses of 6.6 ] 1011È8.0 ] 1014In all runs, the M _ . halos have density cusps proportional to r~1.5 developed at their centers, which is consistent with the results of recent high-resolution calculations. The density structure evolves in a self-similar way and is universal in the sense that it is independent of the halo mass and initial random realization of density Ñuctuation. The density proÐle is in good agreement with the proÐle proposed by Moore et al., which has a central slope proportional to r~1.5 and an outer slope proportional to r~3. The halo grows through repeated accretion of di †use smaller halos. We argue that the cusp is understood as a convergence slope for the accretion of tidally disrupted matter.

show abstract

Section: Other Numerical E †Ectscontrasting

confidence: 58%

Section: Introductionmentioning

confidence: 99%

Structure of Dark Matter Halos from Hierarchical Clustering

Fukushige

Makino

2001

ApJ

201

189

View full text Add to dashboard Cite

show abstract

“…Replacing M v in equation 8, the virial radius is found to be R v = 12 kpc. Using the relationship between M v and the concentration parameter c found in [37] (see also [38]) yields c ≃ 22. Finally r s = 5.35 × 10 −1 kpc is obtained using r s = c/R v .…”

Section: Astrophysical Factor Calculationmentioning

confidence: 91%

H.E.S.S. constraints on dark matter annihilations towards the sculptor and carina dwarf galaxies

Abramowski¹,

Acero²,

Aharonian³

et al. 2011

Astroparticle Physics

View full text Add to dashboard Cite

The Sculptor and Carina Dwarf spheroidal galaxies were observed with the H.E.S.S. Cherenkov telescope array between January 2008 and December 2009. The data sets consist of a total of 11.8 and 14.8 hours of high quality data, respectively. No gamma-ray signal was detected at the nominal positions of these galaxies above 220 GeV and 320 GeV, respectively. Upper limits on the gamma-ray fluxes at 95% C.L. assuming two forms for the spectral energy distribution (a power law shape and one derived from dark matter annihilation) are obtained at the level of 10 −13 to 10 −12 cm −2 s −1 in the TeV range. Constraints on the velocity weighted dark matter particle annihilation cross section for both Sculptor and Carina dwarf galaxies range from σv ∼ 10 −21 cm 3 s −1 down to σv ∼ 10 −22 cm 3 s −1 depending on the dark 3 matter halo model used. Possible enhancements of the gamma-ray flux are studied: the Sommerfeld effect, which is found to exclude some dark matter particle masses, the internal Bremsstrahlung and clumps in the dark-matter halo distributions.

show abstract

“…Within the cold dark matter (CDM) paradigm, ⋆ E-mail: sebastien.peirani@oca.eu earlier works ignoring the effects of gas dissipation and star formation processes, have suggested that dark matter haloes have spherically-averaged density profiles that can be well fitted by simple analytical function such as the NFW profile (Navarro et al 1996a;Navarro et al 1997) in which the inner slope tends to -1 or could even be as steep as -1.5 (e.g. Moore et al 1998;Jing & Suto 2000). Later numerical works favour the Einasto profile with a finite central density though this profile is still cuspy and close to the NFW one (Merritt et al 2006;Stadel et al 2009;Navarro et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

Peirani

Dubois

Volonteri

et al. 2017

Monthly Notices of the Royal Astronomical Society

147

141

View full text Add to dashboard Cite

Using a suite of three large cosmological hydrodynamical simulations, HORIZON-AGN, HORIZON-NOAGN (no AGN feedback) and HORIZON-DM (no baryons), we investigate how a typical sub-grid model for AGN feedback affects the evolution of the inner density profiles of massive dark matter haloes and galaxies. Based on direct object-to-object comparisons, we find that the integrated inner mass and density slope differences between objects formed in these three simulations (hereafter, H AGN , H noAGN and H DM ) significantly evolve with time. More specifically, at high redshift (z ∼ 5), the mean central density profiles of H AGN and H noAGN dark matter haloes tend to be much steeper than their H DM counterparts owing to the rapidly growing baryonic component and ensuing adiabatic contraction. By z ∼ 1.5, these mean halo density profiles in H AGN have flattened, pummelled by powerful AGN activity ("quasar mode"): the integrated inner mass difference gaps with H noAGN haloes have widened, and those with H DM haloes have narrowed. Fast forward 9.5 billion years, down to z = 0, and the trend reverses: H AGN halo mean density profiles drift back to a more cusped shape as AGN feedback efficiency dwindles ("radio mode"), and the gaps in integrated central mass difference with H noAGN and H DM close and broaden respectively. On the galaxy side, the story differs noticeably. Averaged stellar profile central densities and inner slopes are monotonically reduced by AGN activity as a function of cosmic time, resulting in better agreement with local observations.

show abstract

The Density Profiles of the Dark Matter Halo Are Not Universal

Cited by 391 publications

References 24 publications

Structure of Dark Matter Halos from Hierarchical Clustering

Structure of Dark Matter Halos from Hierarchical Clustering

H.E.S.S. constraints on dark matter annihilations towards the sculptor and carina dwarf galaxies

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

Contact Info

Product

Resources

About