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Temperature Structure in Merging Coma Cluster of Galaxies

Published online by Cambridge University Press:  25 May 2016

H. Honda ,
M. Hirayama ,
H. Ezawa ,
K. Kikuchi ,
T. Ohashi ,
M. Watanabe ,
H. Kunieda  and
K. Yamahita
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

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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
Information
Symposium - International Astronomical Union , Volume 188: The Hot Universe , 1998 , pp. 308 - 309
Copyright
Copyright © Kluwer 1998 

References

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