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J.E Krick, R.A. Bernstein (University of Michigan)
We present an update on research into the flux, color, profile shape and substructure of the intracluster star light in a sample of 10 galaxy clusters. This light comes from a population of stars which are no longer bound to their host galaxies due either to stripping from mergers, harassment events, or ram pressure forces in the ICM, or to in situ formation in gas clouds which have been stripped from the galaxies. As such the intracluster stars can be used to study galaxy evolution processes in clusters. We measure a diffuse intracluster component in 2 bands in all 10 clusters in our sample down to surface brightnesses of less than 1% of the sky background. This population accounts for roughly 10 percent of the total cluster light inside of one third of the virial radius. We examine this population of stars as a function of cluster mass, morphology, redshift, and density.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.