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Issue A&A
Volume 420, Number 3, June IV 2004
Page(s) 833 - 845
Section Cosmology (including clusters of galaxies)
DOI http://dx.doi.org/10.1051/0004-6361:20035760



A&A 420, 833-845 (2004)
DOI: 10.1051/0004-6361:20035760

An XMM-Newton study of the RGH 80 galaxy group

Y.-J. Xue1, 2, H. Böhringer1 and K. Matsushita1, 3

1  Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany
2  National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
3  Department of Physics, Tokyo University of Science, 1-3 Kagurazaka, Shinjyuku-ku, Tokyo 162-8601, Japan

(Received 27 November 2003 / Accepted 27 February 2004)

Abstract
We present an X-ray study of the galaxy group RGH 80, observed by XMM-Newton . The X-ray emission of the gas is detected out to ~ 462 h-150 kpc, corresponding to ~ 0.45 r200. The group is relatively gas rich and luminous with respect to its temperature of 1.01  $\pm$ 0.01 keV. Using the deprojected spectral analysis, we find that the temperature peaks at ~ 1.3 keV around  0.11r200, and then decreases inwards to 0.83 keV at the center and outwards to ~ $70\%$ of the peak value at large radii. Within the central ~ 60 kpc of the group where the gas cooling time is less than the Hubble time, a two-temperature model with temperatures of 0.82 and 1.51 keV and the Galactic absorption gives the best fit of the spectra, with ~ $20\%$ volume occupied by the cool component. We also derive the gas entropy distribution, which is consistent with the prediction of cooling and/or internal heating models. Furthermore, the abundances of O, Mg, Si, S and Fe decrease monotonically with radius. With the observed abundance ratio pattern, we estimate that ~ $85\%$ or ~ $72\%$ of the iron mass is contributed by SN Ia, depending on the adopted SN II models.


Key words: galaxies: clusters: individual: RGH 80 -- X-rays: galaxies: clusters

Offprint request: Y.-J. Xue, yxue@mpe.mpg.de

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© ESO 2004


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