The Build-up Of The Red Sequence In Galaxy Clusters Over Half Of Cosmic Time.

Details The Build-up Of The Red Sequence In Galaxy Clusters Over Half Of Cosmic Time. The Build-up Of The Red Sequence In Galaxy Clusters Over Half Of Cosmic Time.

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21537805r&link_type=abstract

American Astronomical Society, AAS Meeting #215, #378.05; Bulletin of the American Astronomical Society, Vol. 42, p.588

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Recent observations have shown that the total mass in L>L* red galaxies has increased by a factor of 2 at z<1, although at different rates as a function of galaxy mass. Despite the advance made by these studies of the whole galaxy population, until recently it has not been clear if the growth of the red sequence depended on environment. To address this question we present the evolution of the red sequence as measured in 16 intermediate redshift clusters drawn from the ESO Distant Cluster Survey (EDisCS). Unlike massive x-ray selected clusters, these clusters have velocity dispersions that make them likely progenitors of clusters that populate the local Universe. Using an SDSS cluster sample we track the evolution of the cluster red sequence over half of cosmic time and compare it to the co-eval field LF. We find that the faint end of the red sequence built up rapidly at z<0.8, and that the evolution was faster in clusters than in the field. There is also a mild dependence of the evolution on the velocity dispersion of the clusters, such that higher velocity dispersion clusters evolve more quickly. We track the growth in the total red light of clusters over time and find that the red sequence must grow by a factor of about 2 in light or mass to match the total luminosities of local clusters. On the other hand, simple but conservative models for how the mass grows results in too much growth over time to match the local clusters. The required growth can only be reconciled with the implied growth if stars are stripped from infalling cluster galaxies and added to the intra-cluster medium.

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