NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-06-19 T02:31:41 PDT
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For refcode 2001PASJ...53..401M:
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NED Abstract

Copyright by Astronomical Society of Japan. 2001PASJ...53..401M X-Ray Probing of the Central Regions of Clusters of Galaxies Kazuo MAKISHIMA, Hajime EZAWA, Yasushi FUKAZAWA, Hirohiko HONDA, Yasushi IKEBE, Tuneyoshi KAMAE, Ken'ich KIKUCHI, Kyoko MATSUSHITA, Kazuhiro NAKAZAWA, Takaya OHASHI, Tadayuki TAKAHASHI, Takayuki TAMURA, and Haiguang XU Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033; maxima@phys.s.u-tokyo.ac.jp Research Center for the Early Universe (RESCEU), The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033 Nobeyama Radio Observatory, National Astronomical Observatory, Minamimaki, Minamisaku, Nagano 384-1305 Department of Physical Science, Hiroshima University, 1-3-1 Kagamiyama, Higashi-hiroshima, Hiroshima 739-8526 The Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 226-8510 Max-Planck-Institut fur extraterrestrische Physik, Postfach 1603, D-85740, Garching, Germany Space Utilization Research Program, National Space Development Agency of Japan, Tsukuba, Ibaraki 305-8505 Department of Physics, Tokyo Metropolitan University, Hachioji, Tokyo 192-0397 SRON, Sorbonnelaan 2, 3584 CA Utrecht, the Netherlands Institute for Space Astrophysics, Shanghai Jiao Tong University, Huashan Road 1954, Shanghai 200030, PRC (Received 2000 September 29; accepted 2001 February 28) Abstract The results on ASCA X-ray study of the central regions of medium-richness clusters of galaxies are summarized, while emphasizing the differences between cD and non-cD clusters. The intra-cluster medium (ICM) is likely to consist of two (hot and cool) phases within ~ 100 kpc of a cD galaxy, where the ICM metallicity is also enhanced. In contrast, the ICM in non-cD clusters appears to be isothermal with a small metallicity gradient right of the center. The gravitational potential exhibits a hierarchical nesting around cD galaxies, while a total mass-density profile with a central cusp is indicated for a non-cD cluster, Abell 1060. The iron-mass-to-light ratio of the ICM decreases toward the center in both types of clusters, although it is radially constant in peripheral regions. The silicon-to-iron abundance ratio in the ICM increases with the cluster richness, but remains close to the solar ratio around cD galaxies. These overall results are interpreted without appealing to the popular cooling-flow hypothesis. Instead, an emphasis is put on the halo-in-halo structure formed around cD galaxies. Key Words: galaxies: clusters: general - ISM: abundances - plasmas - X-rays: galaxies: clusters - X-rays: ISM
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