A&A 452, 397-412 (2006)
DOI: 10.1051/0004-6361:20053864

Chemical evolution in Sérsic 159-03 observed with XMM-Newton

J. de Plaa^{1, 2}, N. Werner¹, A. M. Bykov³, J. S. Kaastra¹, M. Méndez¹, J. Vink^{1, 2}, J. A. M. Bleeker^{1, 2}, M. Bonamente⁴ and J. R. Peterson<sup>5

1</sup>  SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
    e-mail: j.s.kaastra@sron.nl
²  Astronomical Institute, Utrecht University, PO Box 80000, 3508 TA Utrecht, The Netherlands
³  A.F. Ioffe Institute for Physics and Technology, 26 Polytechnicheskaia, 194021 St. Petersburg, Russia
⁴  Department of Physics, University of Alabama, Huntsville, AL 35899, USA
⁵  KIPAC, Stanford University, PO Box 90450, MS 29, Stanford, CA 94039,USA

(Received 20 July 2005 / Accepted 26 February 2006 )

Abstract
Using a new long X-ray observation of the cluster of galaxies Sérsic 159-03 with XMM-Newton, we derive radial temperature and abundance profiles using single- and multi-temperature models. The fits to the EPIC and RGS spectra prefer multi-temperature models especially in the core. The radial profiles of oxygen and iron measured with EPIC/RGS and the line profiles in RGS suggest that there is a dip in the O/Fe ratio in the centre of the cluster compared to its immediate surroundings. A possible explanation for the large scale metallicity distribution is that SNIa and SNII products are released in the ICM through ram-pressure stripping of in-falling galaxies. This causes a peaked metallicity distribution. In addition, SNIa in the central cD galaxy enrich mainly the centre of the cluster with iron. This excess of SNIa products is consistent with the low O/Fe ratio we detect in the centre of the cluster. We fit the abundances we obtain with yields from SNIa, SNII and Population-III stars to derive the clusters chemical evolution. We find that the measured abundance pattern does not require a Population-III star contribution. The relative contribution of the number of SNIa with respect to the total number of SNe which enrich the ICM is about 25-50%. Furthermore, we discuss the possible presence of a non-thermal component in the EPIC spectra. A potential source of this non-thermal emission can be inverse-Compton scattering between Cosmic Microwave Background (CMB) photons and relativistic electrons, which are accelerated in bow shocks associated with ram-pressure stripping of in-falling galaxies.

Key words: galaxies: clusters: general -- galaxies: clusters: individual: Sérsic 159-03 -- galaxies: abundances -- intergalactic medium -- X-rays: galaxies: clusters

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