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Intergalactic Gas

Published online by Cambridge University Press:  07 February 2017

George B. Field
George B. Field*
Affiliation:
Center for Astrophysics, Harvard College Observatory Smithsonian Astrophysical Observatory, Cambridge, Mass., U.S.A.

Abstract

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Evidence that rich clusters of galaxies contain hot (T = 108 K) intracluster gas is reviewed. Such gas contributes little to Ω (0.003) but it has been argued that Ω must be less than 0.05 for true intergalactic gas, if accretion of more gas than is observed in rich clusters is to be avoided. This argument is reviewed.

If the de Vaucouleurs' groups are bound by intracluster gas, T is expected to be 105 to 107 K and the contribution to Ω is ≃ 1. Since the clumping factor C is estimated to be ≃ 7, the resulting value of Ω2C is ≃ 7. This does not violate the observed diffuse soft X-ray background intensity. Gas should be sought in such groups. Smoothly distributed gas with 107 < T < 3 × 108 K and Ω = 1 is not ruled out by direct observations.

Type
Part I: The Contemporary Structure and Dynamics of the Universe
Information
Symposium - International Astronomical Union , Volume 63: Confrontation of Cosmological Theories , 1974 , pp. 13 - 30
Copyright
Copyright © Reidel 1974 

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