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For refcode 1997ApJ...481..660I:
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1997ApJ...481..660I Structure of the X-Ray-emitting Gas in the Hydra A Cluster of Galaxies Y. IKEBE, K. MAKISHIMA, H. EZAWA, Y. FUKAZAWA, M. HIRAYAMA, H. HONDA, Y. ISHISAKI, K. KIKUCHI, H. KUBO, T. MURAKAMI, T. OHASHI, T. TAKAHASHI, AND K. YAMASHITA Received 1996 October 18; accepted 1996 December 31 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 10^9^ 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. Subject headings: galaxies: clusters: individual (Hydra A)-intergalactic medium-X-rays: galaxies
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