Key points are not available for this paper at this time.
The average mass density profile measured in the CNOC cluster survey is well described with the analytic form nu (r) =A/r* (r+a) ², as advocated on the basis on n-body simulations by Navarro, Frenk & White. The predicted core radii are a=0. 20 (in units of the radius where the mean interior density is 200 times the critical density) for an Omega=0. 2 open CDM model, or a=0. 26 for a flat model, with little dependence on other cosmological parameters for simulations normalized to the observed cluster abundance. The measured scale radius of the observed clusters, a=0. 27 (with a 95% confidence range of 0. 13-0. 43), is in excellent agreement with the predicted values. Moreover, the profiles and total masses of the clusters as individuals can be acceptably predicted from the cluster RMS line-of-sight velocity dispersion alone. This is strong support of the hierarchical clustering theory for the formation of galaxy clusters in a cool, collisionless, dark matter dominated universe.
Carlberg et al. (Sun,) studied this question.