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Temperature Structure in Merging Coma Cluster of Galaxies

Published online by Cambridge University Press:  25 May 2016

H. Honda
Affiliation:
The Institute of Space and Astronautical Science, 3-1-1, Yoshinodai, Sagamihara, Kanagawa, 229, Japan
M. Hirayama
Affiliation:
Department of Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113, Japan
H. Ezawa
Affiliation:
Department of Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113, Japan
K. Kikuchi
Affiliation:
Department of Physics, Tokyo Metropolitan University, Hachioji, Tokyo 192-03, Japan
T. Ohashi
Affiliation:
Department of Physics, Tokyo Metropolitan University, Hachioji, Tokyo 192-03, Japan
M. Watanabe
Affiliation:
Department of Physics, Nagoya University, Chikusa-ku, Nagoya 464-01, Japan
H. Kunieda
Affiliation:
Department of Physics, Nagoya University, Chikusa-ku, Nagoya 464-01, Japan
K. Yamahita
Affiliation:
Department of Physics, Nagoya University, Chikusa-ku, Nagoya 464-01, Japan

Extract

The Coma cluster has been recognized as an archetype of rich and relaxed clusters, until recent ROSAT observations reveal that the intracluster medium (ICM) has a complex distribution (Briel et al. 1992; White et al. 1993). The X-ray surface brightness distribution shows a secondary peak around the galaxy NGC 4839, at 40' SW from the cluster center.

Type
Session 1: Plasma and Fresh Nucleosynthesis Phenomena
Copyright
Copyright © Kluwer 1998 

References

1. Briel, U. G., Henry, J. P., and Boehringer, H. 1992, A&A, 259, L31 Google Scholar
2. Evrard, A.E. 1990, Clusters of Galaxies, ed. Oegerle, W.R. (Cambridge: Cambridge Univ. Press), 287 CrossRefGoogle Scholar
3. Honda, H., Hirayama, M., et al. 1996, ApJ, 473, L71 CrossRefGoogle Scholar
4. Hughes, J.P., Butcher, J. A., Stewart, G. C., and Tanaka, Y. 1993, ApJ, 404, 611 CrossRefGoogle Scholar
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6. Hughes, J.P., Gorenstein, P., and Fabricant, D. 1988a, ApJ, 329, 82 CrossRefGoogle Scholar
7. Hughes, J.P., et al. 1988b, ApJ, 327, 615 CrossRefGoogle Scholar
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