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Iron Line Mapping of Cluster of Galaxies and the Effect of ResonanceScattering
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Title:
Structure of the X-Ray--emitting Gas in the Hydra A Cluster of Galaxies
Authors:
Ikebe, Y.; Makishima, K.; Ezawa, H.; Fukazawa, Y.; Hirayama, M.; Honda, H.; Ishisaki, Y.; Kikuchi, K.; Kubo, H.; Murakami, T.; Ohashi, T.; Takahashi, T.; Yamashita, K.
Journal:
Astrophysical Journal v.481, p.660
Publication Date:
05/1997
Origin:
APJ
ApJ Keywords:
GALAXIES: CLUSTERS: INDIVIDUAL NAME: HYDRA A, GALAXIES: INTERGALACTIC MEDIUM, X-RAYS: GALAXIES
Abstract Copyright:
(c) 1997: The American Astronomical Society
Bibliographic Code:
1997ApJ...481..660I

Abstract

The temperature and abundance structure in the intracluster medium (ICM) of the Hydra A Cluster of galaxies is studied with ASCA and ROSAT. The effect of the large extended outskirts in the point-spread function of the X-ray telescope on ASCA is included in this analysis. In the X-ray brightness profile, the strong central excess above a single beta model, identified in the Einstein and ROSAT data, is also found in the harder energy band (>4 keV). A simultaneous fit of five annular spectra taken with the GIS instrument shows a radial distribution of the temperature and metal abundance. A significant central enhancement in the abundance distribution is found, while the temperature profile suggests that the ICM is approximately isothermal, with a temperature of ~3.5 keV. The ROSAT position-sensitive proportional counter (PSPC) spectrum in the central 1.'5 region indicates a significantly lower temperature than the GIS result. A joint analysis of the GIS and PSPC data reveals that the spectra can be described by a two-temperature model as well as by a cooling flow model. In both cases, the hot-phase gas with a temperature of ~3.5 keV occupies more than 90% of the total emission measure within 1.'5 from the cluster center. The estimated mass of the cooler (0.5--0.7 keV) component is ~(2--6) x 109 M&sun;, which is comparable to the mass of hot halos seen in non-cD ellipticals. The cooling flow model gives the mass deposition rate of 60 +/- 30 M&sun; yr-1, an order of magnitude lower than the previous estimation.


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