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X-Ray Studies of Clusters of Galaxies with The Einstein Observatory

Published online by Cambridge University Press:  30 March 2016

D. J. Helfand ,
W. H.-M. Ku  and
F. Abramopoulos
D. J. Helfand
Affiliation:
Columbia Astrophysics Laboratory, Departments of Astronomy and Physics, Columbia University, New York, USA
W. H.-M. Ku
Affiliation:
Columbia Astrophysics Laboratory, Departments of Astronomy and Physics, Columbia University, New York, USA
F. Abramopoulos
Affiliation:
Columbia Astrophysics Laboratory, Departments of Astronomy and Physics, Columbia University, New York, USA

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With the advent of imaging in X-ray astronomy, we can, for the first time, study extended sources with the same detailed spatial and spectral resolution employed by radio and optical astronomers. As in other fields of astronomy, the study of the X-ray emission from clusters of galaxies is beginning to feel the tremendous impact of this advance. The accompanying contributions by Murray and by Grindlay show that the division of clusters into classes based solely on X-ray morphology holds clear implications for the origin of the intracluster medium and the evolution of the cluster as a whole. Comparisons with optical and radio data, along with detailed X-ray studies of nearby objects and the extension of cluster observations to redshifts greater than 0.5, will help connect these ideas to a sound theoretical base. In this report on the cluster observations performed by the Columbia Astrophysics Laboratory with the Einstein Observatory, we restrict ourselves to three brief comments concerning the following areas: (1) The correlation of X-ray brightness with cluster morphology, (2) the detection of a spiral-rich cluster at z ˜ 0.4, and (3) detailed observations of Coma, the nearest rich cluster.

Type
Joint Discussion
Information
Highlights of Astronomy , Volume 5: Highlights of Astronomy. As presented at the XVIIth General Assembly of the IAU, 1979 , 1980 , pp. 747 - 751
Copyright
Copyright © Cambridge University Press 1980

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