EDP Sciences
First Results from XMM-Newton
Free access
Issue
A&A
Volume 365, Number 1, January I 2001
First Results from XMM-Newton
Page(s) L87 - L92
DOI http://dx.doi.org/10.1051/0004-6361:20000038


A&A 365, L87-L92 (2001)
DOI: 10.1051/0004-6361:20000038

X-ray spectroscopy of the cluster of galaxies Abell 1795 with XMM-Newton

T. Tamura1, J. S. Kaastra1, J. R. Peterson2, F. B. S. Paerels2, J. P. D. Mittaz3, S. P. Trudolyubov4, G. Stewart5, A. C. Fabian6, R. F. Mushotzky7, D. H. Lumb8 and Y. Ikebe9.

1  SRON Laboratory for Space Research Sorbonnelaan 2, 3584 CA Utrecht, The Nether lands
2  Astrophysics Laboratory, Columbia University, 550 West 120th Street, New York, NY 10027, USA
3  Department of Space and Climate Physics, University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Surrey, UK
4  NIS-2, Los Alamos National Laboratory, Los Alamos, NM 87545, USA
5  Department of Physics and Astronomy, The University of Leicester, Leicester LE1, UK
6  Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK
7  NASA Goddard Space Flight Center, Code 662, Greenbelt, Maryland 20771, USA
8  Astrophysics Div., European Space Agency, ESTEC, Postbus 299, 2200AG Noordwijk, The Nether lands
9  Max Planck Institut für Extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany

(Received 3 October 2000 / Accepted 17 October 2000)

Abstract
The initial results from XMM-Newton observations of the rich cluster of galaxies Abell 1795 are presented. The spatially-resolved X-ray spectra taken by the European Photon Imaging Cameras (EPIC) show a temperature drop at a radius of $\sim$200 kpc from the cluster center, indicating that the ICM is cooling. Both the EPIC and the Reflection Grating Spectrometers (RGS) spectra extracted from the cluster center can be described by an isothermal model with a temperature of $\sim$4 keV. The volume emission measure of any cool component (< 1 keV) is less than a few % of the hot component at the cluster center. A strong OVIII Lyman $\alpha$ line was detected with the RGS from the cluster core. The O abundance and its ratio to Fe at the cluster center is 0.2-0.5 and 0.5-1.5 times the solar value, respectively.


Key words: galaxies: clusters: individual: Abell 1795 - galaxies: clusters: general -galaxies: cooling flows -X-rays: galaxies

Offprint request: T. Tamura, T.Tamura@sron.nl

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