Statistics of Physical Properties of Dark Matter Clusters

By L. Shaw, Jochen Weller, Jeremiah P. Ostriker, Paul Bode. 2005

182 citations recorded by the source corpus.

We have identified over 2000 well-resolved cluster halos, and also their associated bound subhalos, from the output of a 10243 particle cosmological N-body simulation (of box size 320 h-1 Mpc and softening length 3.2 h-1 kpc). This has allowed us to measure halo quantities in a statistically meaningful way, and for the first time analyze their distribution for a large and well-resolved sample. We characterize each halo in terms of its morphology, concentration, spin, circular velocity, and the fraction of their mass in substructure. We also identify those halos that have not yet reached a state of dynamical equilibrium, using the virial theorem with an additional correction to account for the surface pressure at the boundary. These amount to 3.4% of our initial sample. For the virialized halos, we find a median of 5.6% of halo mass is contained within substructure, with the distribution ranging between no identified subhalos to 65%. The fraction of mass in substructure increases with halo mass with logarithmic slope of 0.44 ± 0.06. Halos tend to have a prolate morphology, becoming more so with increasing mass. Subhalos have a greater orbital angular momentum per unit mass than their host halo. Furthermore, their orbital angular momentum is typically well aligned with that of their host. Overall, we find that dimensionless properties of dark matter halos do depend on their mass, thereby demonstrating a lack of self-similarity.

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

View Paper: https://www.semanticscholar.org/paper/175d0dfb4e77ffa9493d33e7ca088e5fcdce24e6

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Citations in the corpus

Dark matter halo concentrations in the Wilkinson Microwave Anisotropy Probe year 5 cosmology (2008, background): “Because the c(M) relation is very sensitive to the primordial power spectrum (e.g. ENS; Alam, Bullock, & Weinberg 2002; Dolag et al. 2004; Kuhlen et al. 2005), it is not clear whether the MS results accurately describe our Universe.”
Virial Scaling of Massive Dark Matter Halos: Why Clusters Prefer a High Normalization Cosmology (2007, methodology): “Our estimate of 10% for the fraction of strongly interacting halos is somewhat higher than the 3.4% derived by Shaw et al. (2006) in their analysis of a computational sample of 2000 wellresolved ( 104 particle) CDM halos more massive than 3 ; 1013 h 1 M .”
Lensing and x-ray mass estimates of clusters (simulations) (2012, unknown): “Studies based on simulations showed that clusters forming in a CDM framework are generally prolate systems (Shaw et al. 2006; Allgood et al. 2006; Lau et al. 2011).”
Characterization of subhalo structural properties and implications for dark matter annihilation signals (2016, background): “…and different algorithms have been proposed in order to identify small structures within simulated host halos (Ghigna et al. 2000; Weller et al. 2005; Shaw et al. 2006; Springel et al. 2001; Gill et al. 004a,b; Tormen & Moscardini 2004; Giocoli et al. 008b, 2010; Han et al. 2012; Behroozi et al.…”
MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE (2010, result): “In that paper, however, they consider several other simulation results as well, and find similar results in all cases (Shaw et al. 2006; Springel et al. 2001; Tormen et al. 2004; De Lucia et al. 2004; Gao et al. 2004; Nurmi et al. 2006).”
MultiDark simulations: the story of dark matter halo concentrations and density profiles (2014, background): “Typical value of the correction is ∼ 0.2, which is similar to those found by Shaw et al. (2006); Knebe & Power (2008) and Davis et al. (2011).”
CLASH: WEAK-LENSING SHEAR-AND-MAGNIFICATION ANALYSIS OF 20 GALAXY CLUSTERS (2014, background): “For our redshift range 0.187 ≤ z ≤ 0.686, ∆vir ranges approximately from ' 110 to 140 with respect to the critical density of the universe at the cluster redshift. morphology (Shaw et al. 2006).”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. I. Galaxy Mergers and Quasar Activity (2007, background): “…et al. 2004) and an alternative subhalo mass function calculation (van den Bosch et al. 2005, normalized to match cosmological simulations as in Shaw et al. 2006), which brackets the range of a number of different estimates (e.g., Springel et al. 2001; Tormen et al. 2004; De Lucia et al.…”
The dark matter haloes of massive, relaxed galaxy clusters observed with Chandra (2006, methodology): “Although the normalization c0 at 8× 1014 h−1M⊙ and the redshift evolution, b, are consistent with the Shaw et al. (2006) simulations and Dolag et al. (2004) model, the mass-concentration relation is noticeably steeper.”
A Bayesian approach to strong lensing modelling of galaxy clusters (2007, background): “Similarly, N-body simulations of clusters show that the mass distribution of subhalos inside a cluster halo follows a Schechter function (e.g. Shaw et al. 2006).”
DARK MATTER HALO PROFILES OF MASSIVE CLUSTERS: THEORY VERSUS OBSERVATIONS (2011, background): “Previous studies (Jing 2000; Shaw et al. 2006; Neto et al. 2007; Duffy et al. 2008), have fitted the concentration distribution to a log-normal distribution.”
Evolution of the cosmic web (2014, background): “…to reveal that such objects are highly clustered and that they have a very anisotropic spatial distribution, favouring filamentary configurations (Basilakos et al. 2006; Shaw et al. 2006; Wray et al. 2006; Costa-Duarte, Sodré & Durret 2011; Einasto et al. 2011a; Liivamägi, Tempel & Saar 2012).”
Concentration, spin and shape of dark matter haloes as a function of the cosmological model: WMAP1, WMAP3 and WMAP5 results (2008, background): “Although some unrelaxed haloes may have a small xoff , the advantage of this parameter over, for example, the actual virial ratio, 2T/V , as a function of radius (Macciò, Murante & Bonometto 2003; Shaw et al. 2006), is that the former is trivial to evaluate.”
The masses and density profiles of halos in a LCDM galaxy formation simulation (2014, background): “…are well fit by the NFW profile (equation 1) at all redshifts down to a few per cent of the virial radius (Navarro et al. 1997, 2004; Bullock et al. 2001; Eke et al. 2001; Shaw et al. 2006; Macciò et al. 2007; Neto et al. 2007; Duffy et al. 2008; Ludlow et al. 2013; Dutton & Macciò 2014).”
ON THE ACCURACY OF WEAK-LENSING CLUSTER MASS RECONSTRUCTIONS (2010, background): “The inertia tensor is defined as (e.g., Shaw et al. 2006) Mi j = 1 N∆ ∑ n x(n)i x (n) j , (2) where the sum extends over allN∆ particles of the halo within a predefined radiusr∆ andx (n) i is theith coordinate (i = 1,2,3) of the nth particle relative to the halo center.”
Resolving the Formation of Protogalaxies. I. Virialization (2007, background): “3 This is a modified version of the β used in Shaw et al. (2006) to account for kinetic energies and so that it does not diverge when V → 0 in the center.”
The spin and shape of dark matter haloes in the Millennium simulation of a Λ cold dark matter universe (2006, background): “This agrees with previous results (e.g. Warren et al. 1992, Bailin & Steinmetz 2005, Allgood et al. 2006 and Shaw et al. 2006).”
A QUANTITATIVE EXPLANATION OF THE OBSERVED POPULATION OF MILKY WAY SATELLITE GALAXIES (2009, result): “This simple analytic model is able to reproduce the sub-halo mass function, in reasonably good agreement with that found in numerical N -body simulations (Zentner et al. 2005; Shaw et al. 2006; Yoo et al. 2007).”