Cusps in cold dark matter haloes

By Juerg Diemand, Marcel Zemp, B. Moore, Joachim Stadel, M. Carollo, U. Zurich, E. Zurich, University of California Santa Cruz. 2005

173 citations recorded by the source corpus.

We resolve the inner region of a massive cluster forming in a cosmologicalcold dark matter (CDM) simulation with a mass resolution of 2 × 10 6 Mand before z = 4.4 even 3 × 10 5 M� . This is a billion times less than the cluster's final virial mass and a substantial increase over currentCDM simulations. We achieve this resolution using a new multimass refinement procedure and are now able to probe a dark matter halo density profile down to 0.1 per cent of the virial radius. The inner density profile of this cluster halo is well fitted by a power law ρ ∝ r −γ down to the smallest resolved scale. An inner region with roughly constant logarithmic slope is now resolved, which suggests that cuspy profiles describe the inner profile better than recently proposed profiles with a core. The cluster studied here is one out of a sample of six high-resolution cluster simulations, and its inner slope of about γ = 1.2 lies close to the sample average. Ke yw ords: methods: N-body simulations - methods: numerical - galaxies: clusters: general - galaxies: haloes - dark matter.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/5c2ff670d4ee2ef0648c31bdbbcdf1cecd03c6d0

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Citations in the corpus

Cores in warm dark matter haloes: a Catch 22 problem (2012, background): “Secondly, the central densities of CDM haloes in simulations show a cuspy behavior (Moore 1994; Flores & Primack 1994; Diemand et al. 2005; Macciò et al. 2007; Springel et al. 2008), whereas the density profiles inferred from galaxy rotation curves point to a core like structure (e.g. de Blok et…”
On the frequency, intensity, and duration of starburst episodes triggered by galaxy interactions and mergers (2008, background): “…cuspy profiles with a density distribution showing a ρ ∼ r−α behavior, with α ≥ 1, (Cole & Lacey 1996; Navarro et al. 1996, 1997; Avila-Reese et al. 1998; Diemand et al. 2005), numerous studies of the rotation curves of local galaxies have shown that the observational data are more consistent…”
Density profiles of galaxy groups and clusters from SDSS galaxy–galaxy weak lensing (2006, background): “…et al. 2001; Klypin et al. 2001; Fukushige & Makino 2001; Wechsler et al. 2002; Fukushige & Makino 2003; Zhao et al. 2003; Tasitsiomi et al. 2004; Diemand et al. 2005), though with some disagreement in the value of inner asymptotic logarithmic slope, possibly due to resolution issues, and hence…”
Dark Matter Substructure and Gamma-Ray Annihilation in the Milky Way Halo (2006, background): “In comparable runs this problem was observed to give 10% too low local densities at 6 ; 105 crit(z ¼ 0); see Figure 1 of Diemand et al. (2005).”
The impact of dark matter cusps and cores on the satellite galaxy population around spiral galaxies (2010, background): “Subsequent work has confirmed the absence of central-density cores in dark matter simulations (Moore et al. 1999b, Ghigna et al. 2000; Fukushige & Makino 2001; Gao et al. 2004; Navarro 2004; Diemand et al. 2005; Springel et al. 2008a).”
The dark matter haloes of massive, relaxed galaxy clusters observed with Chandra (2006, background): “…consistent view has now emerged in which real dispersion is expected between the inner slopes for individual halos (Klypin et al. 2001; Tasitsiomi et al. 2004) and where typical values for the inner slopes of clusters lie in the range α ∼ 1.1 ± 0.4 (Navarro et al. 2004; Diemand et al. 2004, 2005).”
Redefining the Missing Satellites Problem (2007, background): “For this subhalo, ρ(r = 0.6 kpc) = 1.4 × 108 M⊙/kpc3, so its local density might be underestimated by up to 10%, and the errors in the enclosed mass might be ∼ 20% (Diemand et al. 2005).”
The Orbital Poles of Milky Way Satellite Galaxies: A Rotationally Supported Disk of Satellites (2008, unknown): “5, density profile (Diemand et al. 2005).”
HALO EXPANSION IN COSMOLOGICAL HYDRO SIMULATIONS: TOWARD A BARYONIC SOLUTION OF THE CUSP/CORE PROBLEM IN MASSIVE SPIRALS (2011, background): “N-body simulations predict a central concentration, with a logarithmic slope of≈ −1 (Navarro, Frenk & White 1997, Diemand et al. 2005, Springel et al. 2008).”
The DiskMass Survey VII. The distribution of luminous and dark matter in spiral galaxies (2013, background): “The NFW and similar shapes of the dark-matter halo which have cuspy density profiles with a central slope of ρ ∝ R−1 to ρ ∝ R−1.5, have repeatedly been found in dark-matter-only numerical simulations (e.g., Navarro et al. 1996, 1997; Moore et al. 1999; Klypin et al. 2001; Diemand et al. 2005).”
The Most Dark-Matter-dominated Galaxies: Predicted Gamma-Ray Signals from the Faintest Milky Way Dwarfs (2007, background): “Numerical simulations bound the values of in the range [0.7, 1.2], and the outer slope is approximately 3 (Navarro et al. 2004; Diemand et al. 2005).”
Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, background): “…Frenk, & White 1996a; Navarro, Frenk, & White 1997; Bullock et al. 2001; Eke, Navarro & Steinmetz 2001; Zhao et al. 2003; Navarro et al. 2004; Diemand et al. 2005, 2007; Macciò et al. 2007; Neto et al. 2007; Macciò et al. 2008; Zhao et al. 2009; Navarro et al. 2010; Klypin et al. 2010;…”
THE DENSITY PROFILES OF MASSIVE, RELAXED GALAXY CLUSTERS. I. THE TOTAL DENSITY OVER THREE DECADES IN RADIUS (2012, background): “…to be nearly self-similar, and their detailed structure can be followed in large numerical simulations based only on gravity (e.g., Dubinski & Carlberg 1991; Navarro et al. 1996; Moore et al. 1998; Ghigna et al. 2000; Springel et al. 2005; Diemand et al. 2005; Navarro et al. 2010; Gao et al. 2012).”
HIGH-RESOLUTION ROTATION CURVES AND GALAXY MASS MODELS FROM THINGS (2008, background): “Note that many different parameterizations of CDM halos exist in the literature (e.g., Navarro et al. 1996, 1997; Moore et al. 1999b; Navarro et al. 2004; Diemand et al. 2005).”
The Dark Matter Annihilation Signal from Galactic Substructure: Predictions for GLAST (2008, methodology): “Based on numerical convergence studies (Diemand et al. 2005a) we believe that we can trust the radial density profile of the VL-I host halo down to rconv = 3.4×10−3r200 = 1.3 kpc (Diemand et al. 2007a), corresponding to about 10◦ from the center.”