X-Ray Measurements of Metal Abundances of Hot Gas in Clusters of Galaxies

Details X-Ray Measurements of Metal Abundances of Hot Gas in Clusters of Galaxies X-Ray Measurements of Metal Abundances of Hot Gas in Clusters of Galaxies

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003omeg.conf...77f&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2000. Proceedings of the International Symposium. Held 19-21 January 2000 in Universi

Astronomy and Astrophysics

Astronomy

Scientific paper

Utilizing the imaging spectroscopic capabilities of the Japanease X-ray satellite ASCA, we measured Si and Fe abundances of 40 nearby clusters of galaxies. The spatially averaged Fe abundances of the intracluster medium (ICM) are 0.2-0.3 solar, with only weak dependence on the temperature of the intracluster medium, hence on the cluster richness. In contrast, the spatially averaged Si abundance is observed to increase from 0.3 to 0.6-0.7 solar from the poorer to richer clusters. These results suggest that the supernovae of both type-Ia and type-II significantly contribute to the metal enrichment of the intracluster medium, with the relative contribution of type-II supernovae increasing towards richer clusters. Many clusters exhibit a central increment in the Fe abundance, which is more pronounced in lower temperature clusters; +(0.1-0.2) solar at kT > 5 keV, while +(0.2-0.3) solar at 1.5 < kT < 4 keV. These central excess metals are thought to be ejected from cD galaxies. Several low temperature cD type clusters also show significant Si abundance increase by +(0.1-0.2) solar at the central region. Compared with the Si-rich abundances observed in outer regions of rich clusters, the Si to Fe abundance ratio of central excess metals tends to be near the solar ratio, implying that type Ia products from cD galaxies are dominant in the central excess metals.

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