Dynamics of rich clusters of galaxies. II. The Perseus cluster

The dynamics of the Perseus cluster are analyzed using self-consistent equilibrium analytical models. Using existing data in the literature plus new radial velocities reported here, composite surface density and velocity dispersion profiles are derived. These profiles have been compared with dynamical models described by Kent and Gunn. The best fits suggest the presence of a significant degree of anisotropy in the velocity distribution: galaxy orbits are constrained to pass within a radius of 7r/sub c/ , or 1.03, of the cluster center. For H0 = 50, we find a core radius of 340 kpc (11') and a mass to visual light ratio M/L = 300. Using these results we reanalyze x-ray observations of the intracluster medium in Perseus. A previously noted discrepancy between the observed temperature of the hot gas and the cluster velocity dispersion is reduced but not eliminated. A cooling accretion flow previously deduced to exist in this cluster is shown to extend to only approx.1/3r/sub c/