Diffuse Optical Light in Galaxy Clusters I: Abell 3888
  We are undertaking a program to measure the characteristics of the intracluster light (total flux, profile, color, and substructure) in a sample of 10 galaxy clusters with a range of cluster mass, morphology, and redshift. We present here the methods and results for the first cluster in that sample, A3888. We have identified an intracluster light (ICL) component in A3888 in V and r that contains 13\pm5% of the total cluster light and extends to 700h_{70}^{-1}kpc (~0.3 r_{200}) from the center of the cluster. The ICL color in our smallest radial bin is V-r = 0.3 \pm 0.1, similar to the central cluster ellipticals. The ICL is redder than the galaxies at 400 < r < 700h_{70}^{-1}kpc although the uncertainty in any one radial bin is high. Based on a comparison of V-r color with simple stellar models, the ICL contains a component which formed more than 7 Gyr ago (at z > 1), coupled with a high metallicity (1.0Z_{\odot} < Z_{ICL} \la 2.5Z_{\odot}), and a more centralized component which contains stars formed within the past 5 Gyr (at z ~ 1). The profile of the ICL can be roughly fit by a shallow exponential in the outer regions and a steeper exponential in the central region. We also find a concentration of diffuse light around a small group of galaxies 1.4h_{70}^{-1}Mpc from the center of the cluster. In addition, we find 3 low surface brightness features near the cluster center which are blue (V-r = 0.0) and contain a total flux of 0.1M*. Based on these observations and X-ray and galaxy morphology, we suggest that this cluster is entering a phase of significant merging of galaxy groups in the core, whereupon we expect the ICL fraction to grow significantly with the formation of a cD galaxy as well as the in-fall of groups. 
J. E. Krick (1), R. A. Bernstein (1), and K. A. Pimbblet (2) ((1)   University of Michigan, (2) University of Queensland)