AAS 203rd Meeting, January 2004
Session 61 Galaxy Clusters and Large Scale Structure II
Oral, Tuesday, January 6, 2004, 10:00-11:30am, Centennial III

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[61.04] Cluster Substructure and its Evolution with Redshift

T.E. Jeltema, C.R. Canizares, M.W. Bautz (M.I.T.), D.A. Buote (University of California, Irvine)

Using Chandra archival data, we quantify the evolution of cluster morphology with redshift. To quantify cluster morphology, we use the power ratio method developed by Buote and Tsai (1995). Power ratios are constructed from moments of the two-dimensional gravitational potential and are, therefore, related to a cluster's dynamical state. Our sample includes 40 clusters from the Chandra archive with redshifts between 0.11 and 0.89. These clusters were selected from two fairly complete flux-limited X-ray surveys (the ROSAT Bright Cluster Sample and the Einstein Medium Sensitivity Survey), and additional high-redshift clusters were selected from recent ROSAT flux-limited surveys. Fourteen of the clusters in our sample have redshifts above 0.5, and we see increased structure in these high-redshift clusters. The amount of structure in clusters and its evolution with redshift depend on cosmology, and we plan to compare the observed evolution to the evolution predicted from numerical cluster simulations. This work was supported by NASA.

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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.