Diffuse optical light in galaxy clusters. II. Correlations with cluster properties

作者：Krick J E^*; Bernstein R A

来源：Astronomical Journal, 2007, 134(2): 466-493.

DOI：10.1086/518787

• cosmology : observations
• galaxies : clusters : individual (Abell 141, Abell 2556, Abell 2734
• Abell 3880, Abell 3888, Abell 3984, Abell 4010, Abell 4059, AC 114, AC 118)
• galaxies : evolution
• galaxies : interactions
• galaxies : photometry

We have measured the flux, profile, color, and substructure in the diffuse intracluster light (ICL) in a sample of 10 galaxy clusters with a range of mass, morphology, redshift, and density. Deep, wide-field observations for this project were made in two bands at the 1 m Swope and 2.5 m du Pont telescopes at Las Campanas Observatory. Careful attention in reduction and analysis was paid to the illumination correction, background subtraction, point-spread function determination, and galaxy subtraction. ICL flux is detected in both bands in all 10 clusters ranging from 7.6 x 10(10) to 7.0 x 10(11) h(70)(-1) L(circle dot) in r and 1.4 x 10(10) to 1.2 x 10(11) h(70)(-1) L(circle dot) in the B band. These fluxes account for 6%-22% of the total cluster light within one-quarter of the virial radius in r and 4%-21% in the B band. Average ICL B-r colors range from 1.5 to 2.8 mag when k- and evolution corrected to the present epoch. In several clusters we also detect ICL in group environments near the cluster center and up to 1 h-(-1)(70) Mpe distant from the cluster center. Our sample, having been selected from the Abell sample, is incomplete in that it does not include high-redshift clusters with low density, low flux, or low mass, and it does not include low-redshift clusters with high flux, high mass, or high density. This bias makes it difficult to interpret correlations between ICL flux and cluster properties. Despite this selection bias, we do find that the presence of a cD galaxy corresponds to both centrally concentrated galaxy profiles and centrally concentrated ICL profiles. This is consistent with ICL either forming from galaxy interactions at the center or forming at earlier times in groups and later combining in the center.

• 出版日期2007-8