The dynamics of rich clusters of galaxies. II - The Perseus cluster

Details The dynamics of rich clusters of galaxies. II - The Perseus cluster The dynamics of rich clusters of galaxies. II - The Perseus cluster

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983aj.....88..697k&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 88, June 1983, p. 697-708.

Astronomy and Astrophysics

Astronomy

125

Astrodynamics, Astronomical Models, Galactic Clusters, Galactic Structure, Intergalactic Media, X Ray Sources, Accretion Disks, Celestial Mechanics, Density Distribution, High Temperature Gases, Interstellar Gas, Mass To Light Ratios, Radial Velocity, Red Shift, Spatial Distribution, Velocity Distribution

Scientific paper

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 (1982). The best fit suggest the presence of a significant degree of anisotropy in the velocity distribution: galaxy orbits are constrained to pass within a radius of seven cluster radii, or 1.3 deg of the cluster center. For Hubble constant = 50, a core radius of 340 kpc 11 arcmin and a mass to visual light ratio M/L = 300 are found. Using these results, X-ray observations of the intracluster medium in Perseus are reanalyzed. 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 about one-third of the cluster radius.

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