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JD2 - Diffuse Light in Galaxy Clusters

Published online by Cambridge University Press:  21 October 2010

Magda Arnaboldi  and
Ortwin Gerhard
Magda Arnaboldi
Affiliation:
European Southern Observatory, Karl Schwarzschild-Str 2, 85748 Garching, Germany email: marnabol@eso.org
Ortwin Gerhard
Affiliation:
Max Planck Institute for Extraterr. Physics, Giessenbachstrasse, 85748 Garching, Germany email: gerhard@mpe.mpg.de
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Abstract

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Diffuse intracluster light (ICL) has now been observed in nearby and in intermediate redshift clusters. Individual intracluster stars have been detected in the Virgo and Coma clusters and the first color-magnitude diagram and velocity measurements have been obtained. Recent studies show that the ICL contains of the order of 10% and perhaps up to 30% of the stellar mass in the cluster, but in the cores of some 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 is the connection to the central brightest cluster galaxy? Cosmological N-body and hydrodynamical simulations are beginning to make predictions for the kinematics and origin of the ICL. The ICL traces the evolution of baryonic substructures in dense environments and can thus be used to constrain some 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.

Keywords

(cosmology:) large-scale structure of universegalaxies: clusters: generalgalaxies: evolutiongalaxies: interactionsgalaxies: structuregalaxies: kinematics and dynamicsgalaxies: star clusters(ISM:) planetary nebulae: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 97 - 110
Copyright
Copyright © International Astronomical Union 2010

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