Probing Evolution of Hot Gas and Galaxy Distributions in Galaxy Clusters

Details Probing Evolution of Hot Gas and Galaxy Distributions in Galaxy Clusters Probing Evolution of Hot Gas and Galaxy Distributions in Galaxy Clusters

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009cfdd.confe.120i&link_type=abstract

Chandra's First Decade of Discovery, Proceedings of the conference held 22-25 September, 2009 in Boston, MA. Edited by Scott Wo

Computer Science

Clusters Of Galaxies

Scientific paper

How have spatial distributions of components in galaxy clusters (dark matter, hot gas, metals and galaxies) evolved over the history of the universe? It is commonly known that cluster hot gas distribution is more extended than that of dark matter (beta in the beta model is less than unity for hot gas distribution), which means that the hot gas has higher specific energy than dark matter. In a study of 12 clusters with XMM-Newton (Kawaharada et al. 2009, ApJ, 691, 971), we have found that galaxy luminosity distributions are more centrally-concentrated than corresponding metal distributions in their central 100 kpc regions. One simple interpretation of the result is that galaxies have gradually fallen to the cluster center and merged into a single central galaxy while providing metals to surrounding hot gas, and that kinetic energy lost from galaxies (by interactions of interstellar media and intergalactic hot gas) has expanded the cluster hot gas distribution. If the scenario is correct, the relative distribution of galaxies to hot gas should change/evolve with redshifts. To see this phenomenon, we have started a project to compare distributions of galaxies and hot gas in galaxy clusters at different redshifts. We are utilizing optical data from the Sloan Digital Sky Survey, while those in X-rays from XMM-Newton. Some preliminary results will be presented in the Symposium.

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