Intergalactic stars in z~0.25 galaxy clusters: systematic properties from stacking of Sloan Digital Sky Survey imaging data

Details Intergalactic stars in z~0.25 galaxy clusters: systematic properties from stacking of Sloan Digital Sky Survey imaging data Intergalactic stars in z~0.25 galaxy clusters: systematic properties from stacking of Sloan Digital Sky Survey imaging data

2005-01-11

arxiv.org/abs/astro-ph/0501194v1

Mon.Not.Roy.Astron.Soc.358:949-967,2005

Astronomy and Astrophysics

Astrophysics

21 pages, 12 figures. Accepted for publication in MNRAS. Figures 3 and 4 degraded. Full resolution paper available at http:/

Scientific paper

10.1111/j.1365-2966.2005.08817.x

We analyse the spatial distribution and colour of the intracluster light (ICL) in 683 clusters of galaxies between z=0.2 and 0.3, selected from approx 1500 deg^2 of the SDSS-DR1. Surface photometry in the g, r and i bands is conducted on stacked images of the clusters, after rescaling them to the same metric size and masking out resolved sources. We are able to trace the average surface brightness profile of the ICL out to 700 kpc, where it is less than 1/10,000 of the mean surface brightness of the dark night sky. The ICL appears as a clear surface brightness excess with respect to an inner R^1/4 profile which characterises the mean profile of the BCG. The surface brightness (SB) of the ICL ranges from 27.5 mag/arcsec^2 at 100 kpc to roughly 32 at 700 kpc in the observed r-band (26.5 to 31 in the rest-frame g-band). We find that, on average, the ICL contributes only a small fraction of the total optical emission in a cluster (10.9+-5.0% within 500 kpc). The radial distribution of the ICL is more centrally concentrated than that of the cluster galaxies, but the colours of the two components are identical within the statistical uncertainties. In the mean the ICL is aligned with and more flattened than the BCG itself. This alignment is substantially stronger than that of the cluster light as a whole. The SB of the ICL correlates both with BCG luminosity and with cluster richness, while the fraction of the total light in the ICL is almost independent of these quantities. These results support the idea that the ICL is produced by stripping and disruption of galaxies as they pass through the central regions of clusters. Our measurements of the diffuse light also constrain the faint-end slope of the cluster LF. Slopes alpha<-1.35 would imply more light from undetected galaxies than is observed in the diffuse component.

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