Volume 365, Number 1, January 2001
First Results from XMM-Newton
|Page(s)||L104 - L109|
|Published online||15 January 2001|
X-ray imaging-spectroscopy of Abell 1835
Columbia Department of Physics and Astrophysics Laboratory, 550 W 120th St., New York, NY 10027, USA
2 SRON Laboratory for Space Research Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
3 CEA/DSM/DAPNIA Saclay, Service d'Astrophysique, L'Orme des Merisiers, Bât. 709, 91191 Gif-sur-Yvette, France
4 Max-Planck-Institut für extraterrestrische Physik, PO Box 1312, 85741 Garching, Germany
5 Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK
6 NASA/GFSC, Code 662, Greenbelt, MD, 20771, USA
7 Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
8 Mullard Space Science Laboratory, UCL, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK
Corresponding author: J. R. Peterson, firstname.lastname@example.org
Accepted: 2 November 2000
We present detailed spatially-resolved spectroscopy results of the observation of Abell 1835 using the European Photon Imaging Cameras (EPIC) and the Reflection Grating Spectrometers (RGS) on the XMM-Newton observatory. Abell 1835 is a luminous (1046 ergs ), medium redshift (), X-ray emitting cluster of galaxies. The observations support the interpretation that large amounts of cool gas are present in a multi-phase medium surrounded by a hot ( keV) outer envelope. We detect O VIII Lyα and two Fe XXIV complexes in the RGS spectrum. The emission measure of the cool gas below keV is much lower than expected from standard cooling-flow models, suggesting either a more complicated cooling process than simple isobaric radiative cooling or differential cold absorption of the cooler gas.
Key words: galaxy clusters: individual: Abell 1835 / galaxies: cooling flows / techniques: spectroscopic
© ESO, 2001
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