Redshift Evolution in the Iron Abundance of the Intracluster Medium

Details Redshift Evolution in the Iron Abundance of the Intracluster Medium Redshift Evolution in the Iron Abundance of the Intracluster Medium

2009-04-06

arxiv.org/abs/0904.1007v1

Astrophys.J.698:317-323,2009

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

Scientific paper

10.1088/0004-637X/698/1/317

Clusters of galaxies provide a closed box within which one can determine the chemical evolution of the gaseous baryons with cosmic time. We studied this metallicity evolution in the hot X-ray emitting baryons through an analysis of XMM-Newton observations of 29 galaxy clusters in the redshift range 0.3 < z < 1.3. Taken alone, this data set does not show evidence for significant evolution. However, when we also include a comparable sample of 115 clusters observed with Chandra (Maughan et al. 2008) and a lower redshift sample of 70 clusters observed with XMM at z < 0.3 (Snowden et al. 2008), there is definitive evidence for a decrease in the metallicity. This decrease is approximately a factor of two from z = 0 to z \approx 1, over which we find a least-squares best-fit line Z(z) / Z_{\odot} = (0.46 \pm 0.05) - (0.38 \pm 0.03)z. The greatest uncertainty in the evolution comes from poorly constrained metallicities in the highest redshift bin.

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