Structure of Dark Matter Halos from Hierarchical Clustering

By T. Fukushige, J. Makino. 2000

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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 × 1011-8.0 × 1014 M☉. In all runs, the 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 fluctuation. The density profile is in good agreement with the profile 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 diffuse smaller halos. We argue that the cusp is understood as a convergence slope for the accretion of tidally disrupted matter.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/b7050b07c716bde762f258e598f89a155e22b9a4

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Citations in the corpus

GHASP: an Hα kinematic survey of spiral and irregular galaxies – V. Dark matter distribution in 36 nearby spiral galaxies (2007, background): “…favor cuspy dark halos, although the value of the inner slope γ of the radial density profile, where ρ ∝ r γ (see equation 6 of section 4) depends on the authors, with γ = -1.5 for Moore et al. 1999 as well as Fukushige & Makino 2001 or -1.0 for Navarro, Frenk & White 1997 (hereafter NFW).”
Density profiles of galaxy groups and clusters from SDSS galaxy–galaxy weak lensing (2006, background): “…et al. 1999; Ghigna et al. 2000; Jing & Suto 2000; Bullock 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…”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, background): “…matter haloes has been studied extensively over the past decade and a half using computer simulations (Dubinski & Carlberg 1991; Navarro, Frenk & White 1996, 1997; Moore et al. 1998; Fukushige & Makino 1997, 2001; Klypin et al. 2001; Power et al. 2003; Hayashi et al. 2004; Navarro et al. 2004).”
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).”
On the life and death of satellite haloes (2003, background): “…the detailed study of the internal dynamical evolution of many haloes requires a high number of particles in order to resolve substructure avoiding its artificial evaporation (Moore et al. 1996; Ghigna et al. 1998; Moore et al. 1999b; Lewis et al. 2000; Jing & Suto 2000; Fukushige & Makino 2001).”
LoCuSS: Subaru Weak Lensing Study of 30 Galaxy Clusters (2009, background): “…matter (CDM) model of structure formation is that dark matter halos can be described by a universal mass density profile, as found by Navarro, Frenk, and White (1996, 1997, hereafter NFW; also see Moore et al. 1999; Fukushige & Makino 2001; most recently Navarro et al. 2010 and references therein).”
Formation and Evolution of Galaxy Dark Matter Halos and Their Substructure (2007, background): “…the highly non-linear formation of cold dark matter (CDM) halos and their substructure in great detail (e.g. Ghigna et al. 1998, 2000; Klypin et al. 1999; Moore et al. 1999, 2001; Fukushige et al. 2004; Kravtsov et al. 2004; Diemand et al. 2004; Gao et al. 2004; Gill et al. 2005; Reed et al. 2005).”
Triaxial Modeling of Halo Density Profiles with High-Resolution N-Body Simulations (2002, background): “…fits to the simulation data more carefully, however, α = 1 works better for the halos of cluster mass and α = 1.5 better for those of galactic mass, which is consistent with the finding of Jing & Suto (2000) in the spherical model (but see Fukushige & Makino 2001, for a different point of view).”
Resolving the Structure of Cold Dark Matter Halos (2000, methodology): “Most recently, Fukushige & Makino (2001) simulated 12 halos with masses ranging from 4.3 × 1011 M⊙ to 7.9 × 10 14 M⊙, again with resolution similar to the resolution of simulations presented here.”
There's no place like home? Statistics of Milky Way-mass dark matter haloes (2009, background): “Many studies have shown that halo growth occurs inside-out, with the central regions built up first and the outskirts assem- c© 2010 RAS, MNRAS 000, 1–19 bled later (e.g., Fukushige & Makino 2001; Loeb & Peebles 2003; Zhao et al. 2003b; Diemand et al. 2007; Cuesta et al. 2008).”
Dynamical insight into dark matter haloes (2005, background): “Subsequently, several studies have argued for a somewhat steeper central cusp (e.g. Fukushige & Makino 1997, 2001; Ghigna et al. 1998, 2000; Moore et al. 1998, 1999), with one recent suite of high-resolution simulations appearing to imply γ 0 1.16 ± 0.14 (Diemand, Moore & Stadel 2004b).”
Baryonic pinching of galactic dark matter halos (2006, background): “[1, 2, 3, 4, 5, 6]) , but one would expect the baryonic component of the galaxy to behave very differently since it is able to cool (dissipate energy), and contract considerably.”
The redshift dependence of the structure of massive Λ cold dark matter haloes (2007, background): “…preoccupation concerns indications that halo profiles deviate slightly but systematically from the NFW model (Moore et al. 1998, Jing & Suto 2000, Fukushige & Makino 2001, Navarro et al. 2004, Prada et al. 2006, Merritt et al. 2006), raising the possibility that estimating concentrations by…”
Semianalytical Model of Galaxy Formation with High-Resolution N-Body Simulations (2004, background): “…parameters are very similar to those adopted in many high-resolution resimulations of individual cluster halos (Moore et al. 1999; Jing & Suto 2000; Fukushige & Makino 2001, 2003; Power et al. 2003; Diemand et al. 2004), we have achieved a resolution that can resolve subhalos within massive halos.”
Detailed cluster lensing profiles at large radii and the impact on cluster weak lensing studies (2011, methodology): “Based on the detailed analysis of Fukushige & Makino (2001), we estimate that density profiles are reliable down to ∼ 0.08rvir for our N-body simulations in which N ∼ 104 particles are included in each halo analysed in the present paper.”