Dynamical insight into dark matter haloes

By W. Dehnen, D. McLaughlin. 2005

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We investigate, using the spherical Jeans equation, self-gravitating dynamical equilibria satisfying a relation ρ/σ 3 ∝ r −α , which holds for simulated dark matter haloes over their whole resolved radial range. Considering first the case of velocity isotropy, we find that this problem has only one solution for which the density profile is not truncated or otherwise unrealistic. This solution occurs only for a critical value of αcrit = 35/18 = 1.94, which is consistent with the empirical value of 1.9 ± 0.05. We extend our analysis in two ways: first, we introduce a par ,

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/f2bd6555020a8ef5a9a13fe22f482181b450a4bb

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In Statistical and Nonlinear Physics

Citations in the corpus

The diversity and similarity of simulated cold dark matter haloes (2008, methodology): “For example, Merritt et al. (2006) compared N-body halos with the 3- parameter Einasto formula, as well as with the anisotropic model of Dehnen & McLaughlin (2005) and with the deprojected Sersic (1968) model of Prugniel & Simien (1997).”
Quantifying the heart of darkness with GHALO – a multibillion particle simulation of a galactic halo (2008, background): “It has been pointed out (Taylor & Navarro 2001; Dehnen 2005; Dehnen & McLaughlin 2005) that the phase-space density (PSD) proxy, ρσ−3 vs R is a power-law for CDM haloes, and several new fitting functions for the density profile have been proposed using this fact as a starting point such as the…”
CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 galaxy cluster MACS J1206.2-0847 (2013, methodology): “Dehnen & McLaughlin (2005) have shown that the shape of the density profiles of cosmological halos follows analytically from the power-law behavior ofQ(r) if the system obeys the Jeans equation of dynamical equilibrium (Binney & Tremaine 1987), and if a linearγ-β relation holds, with β(r) = 1− σ2 θ…”
Empirical Models for Dark Matter Halos. II. Inner Profile Slopes, Dynamical Profiles, and ρ/σ3 (2006, methodology): “…in Figures 4 and 5, it would have implied an outer logarithmic slope in the density profile that decayed in an oscillary manner about a value of −2 (Dehnen & McLaughlin 2005, their figure 2), at odds with the data in Figure 3 from Paper I This can be appreciated in Figures 6 and 7 which show the…”
The dark matter haloes of massive, relaxed galaxy clusters observed with Chandra (2006, background): “Recent analytical and numerical work to solve the Jeans equation suggests a value for the inner slope of α ≈ 0.8 (Austin et al. 2005; Dehnen & McLaughlin 2005; Hansen & Stadel 2006).”
Cosmological Simulations with Self-Interacting Dark Matter I: Constant Density Cores and Substructure (2012, methodology): “…= (ρCDM(r)/Q(r)) 1/3 and using a phase-space density profileQ(r) = Q(rs)(r/rs)−η (Taylor & Navarro 2001; Rasia et al. 2004; Ascasibar et al. 2004; Dehnen & McLaughlin 2005; Ascasibar & Gottlöber 2008), we may fully specify thedependence ofr1 on the cross-section and halo parameters (sayVmax…”
A Universal density slope - velocity anisotropy relation for relaxed structures (2004, methodology): “Recently it has indeed been confirmed that the velocity distribution function for the radial and tangential part indeed can be described by using different q’s as suggested above (Hansen et al. 2005).”
Empirical Models for Dark Matter Halos. I. Nonparametric Construction of Density Profiles and Comparison with Parametric Models (2005, methodology): “The parameter α controls the sharpness of the transition (see Zhao et al. 1996; Kravtsov et al. 1998; and equations (37) and (40b) in Dehnen & McLaughlin 2005).”
The redshift dependence of the structure of massive Λ cold dark matter haloes (2007, background): “Taylor & Navarro (2001), Austin et al (2005) and Dehnen & McLaughlin (2005) investigated a halo model based on the assumption that the phase space density, ρ/σ3, was a simple powerlaw of radius.”
Numerical simulations of the dark universe: State of the art and the next decade (2012, background): “84, even though neither the density nor the velocity dispersion profiles by themselves are [32, 38–40].”