Diffuse
intracluster light (ICL) has now been observed in nearby and in
intermediate redshift clusters. Individual intracluster stars have been
detected in the Virgo, Hydra, and Coma clusters (<see
here>) and the first color-magnitude diagram (<see
here>) and velocity measurements have been obtained (<more here>).
Recent studies show that the ICL contains of the order of 10% and
perhaps up to 30% of the mass in stars of the cluster, but in the cores
of more dense and rich clusters like Coma, the local ICL fraction
can be high as 40%-50%.What can we learn from the ICL about the formation of galaxy clusters and the evolution of cluster galaxies? How and when did the ICL form? What are the dominant processes: tidal stripping, disruption, mergers? What is the connection to the central brightest cluster galaxy? Cosmological N-body and hydrodynamical simulations are now beginning to make predictions for the kinematics and origin of the ICL. The evolution of baryonic substructures in dense environments is traced by the ICL which can thus be used to constrain those aspects of cosmological simulations that are most uncertain, such as the modeling of star formation and the mass distribution of the baryonic component in galaxies. The first conference dedicated to the ICL was the Joint Discussion 2 at the General Assembly of the IAU at Rio de Janeiro in August 2009. A link to the webpage with the scientific program and the summary article by the co-organizers can be found <here>. Separate pages summarize our recent work on the kinematics of intracluster stars and what can be learnt from them about galaxies in their cluster environments (<see here>). An introductory summary article can be found here in <English> or <German>. |
Diffuse Light in Galaxy Clusters JD2: XXVII IAU General Assembly Rio de Janeiro - August 6-7, 2009 ![]() ![]() |
![]() The Coma Cluster ![]() [pdf] |
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