XMM Observations of Metal Abundances in the Intracluster Medium

Details XMM Observations of Metal Abundances in the Intracluster Medium XMM Observations of Metal Abundances in the Intracluster Medium

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005omeg.conf...71m&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2003. Held 17-19 November 2003 in RIKEN, Wako, Saitama, Japan. Edited by M Terasawa,

Astronomy and Astrophysics

Astronomy

Scientific paper

Based on XMM-Newton observations of the X-ray halo of M 87 and the Centaurus cluster, abundance profiles of O, Mg, Si, and Fe of the intracluster medium (ICM) are derived. The abundances of Si and Fe show strong decreasing gradients. In contrast, the O and Mg abundances are about a half of the Si abundance at the center. From the gas mass to stellar mass ratio and the comparison of Mg abundance with the stellar metallicity, the stellar mass loss from the central galaxies is indiated to be the main source of the gas in the very central region of the clusters. The observed O, Si and Fe abundance pattern determines the contribution of supernova (SN) Ia and SN II, with the abundance pattern of ejecta of SN Ia. The most of Si and Fe of the ICM in the central region of the clusters come from SN Ia occured in the central galaxies. In order to explain the observed O/Si ratio of a half solar, SN Ia products should have similar abundances of Si and Fe, which may reflect dimmer SN Ia observed in old stellar systems. The Mg/O ratio are close to those of Galactic stars, which indicates that nucleosynthesis of these elements has no discrepancy between our Galaxy and early-type galaxies.

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