Cluster dynamics and cluster masses

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dc.contributor.author Merritt, David en_US
dc.contributor.author Gebhardt, Karl en_US
dc.date.accessioned 2006-03-30T18:24:57Z en_US
dc.date.available 2006-03-30T18:24:57Z en_US
dc.date.issued 1995 en_US
dc.identifier.isbn 2-86332-167-6 en_US
dc.identifier.uri http://hdl.handle.net/1850/1479 en_US
dc.description "Clusters of Galaxies.": Proceedings of the XXIXth Rencontre de Moriond meeting held in Méribel, Savoie, France: 12-19 March 1994. en_US
dc.description Archived in: astro-ph/9510091 18 Oct 1995 AND Rutgers Astrophysics Preprint Series No. 150. en_US
dc.description.abstract 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). en_US
dc.format.extent 320683 bytes en_US
dc.format.mimetype application/pdf en_US
dc.language.iso en_US en_US
dc.publisher Editions Frontières: Moriond Astrophysics Meetings en_US
dc.subject Galaxy clusters en_US
dc.subject Galaxy orbital velocities en_US
dc.title Cluster dynamics and cluster masses en_US
dc.type Proceedings en_US

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