In spite of the promise of new techniques for constraining the mass distribution in galaxy clusters, much remains to be learned from galaxy orbital velocities. This article reviews the theory of potential estimation in hot dynamical systems like galaxy clusters. An analysis is presented of the Coma cluster, based on a sample of ~1500 galaxies with probable membership, of which ~450 have measured velocities. The Coma data are shown to be consistent with a model in which the dark matter density falls roughly as r3 inside of ~1.5 Mpc (H0 = 50), with, perhaps, a transition to a slower falloff at larger radii. We find no signicant evidence for a core in either the galaxy number densities or the mass distribution (Refer to PDF file for exact formulas).

Date of creation, presentation, or exhibit



"Clusters of Galaxies.": Proceedings of the XXIXth Rencontre de Moriond meeting held in Méribel, Savoie, France: 12-19 March 1994.||Archived in: astro-ph/9510091 18 Oct 1995 AND Rutgers Astrophysics Preprint Series No. 150. ISBN: 2-86332-167-6Note: imported from RIT’s Digital Media Library running on DSpace to RIT Scholar Works in February 2014.

Document Type

Conference Proceeding

Department, Program, or Center

School of Physics and Astronomy (COS)


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