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Title:
What is the Virial Radius of a Galaxy Cluster?
Authors:
Opher, R.
Affiliation:
AA(Instituto Astronomico e Geofisico - IAG/USP, Av. Miguel Stefano, 4200 CEP 04301-904 Sao Paulo, S.P., Brazil, )
Publication:
Abstracts of the 19th Texas Symposium on Relativistic Astrophysics and Cosmology, held in Paris, France, Dec. 14-18, 1998. Eds.: J. Paul, T. Montmerle, and E. Aubourg (CEA Saclay), meeting abstract.
Publication Date:
12/1998
Origin:
AUTHOR
Bibliographic Code:
1998tx19.confE.533O

Abstract

Taking into account only gravitational interactions, the virialization radius should be the radius containing matter at 200 times the ambient density, r200. This radius has been used to obtain OmegaM (e.g., Carlberg et al. 1997). However, detailed analysis indicates that only at a radius r500, is there hydrostatic support by thermal pressure (Evrard et al. 1996). We study the value of the virial radius as a function of relevant physical processes such as infall rate, ion and electron thermalization times, central magnetic fields and MHD turbulence.
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