1304.3335 (Tracy Webb et al.)

The Evolution of Dusty Star formation in Galaxy Clusters to z = 1: Spitzer IR Observations of the First Red-Sequence Cluster Survey    [PDF]

Tracy Webb, Daniel O'Donnell, Howard K. C. Yee, David Gilbank, Kristen Coppin, Erica Ellingson, Ashley Faloon, James E. Geach, Mike Gladders, Allison Noble, Adam Muzzin, Gillian Wilson, Renbin Yan

We present an IR study of high-redshift galaxy clusters with the MIPS camera on the Spitzer Space Telescope. Employing a sample of 42 clusters from the RCS-1 over the redshift range 0.3 < z < 1.0 and spanning an approximate range in mass of 10^{14-15} Msun, we show the number of IR-luminous galaxies in clusters above a fixed IR luminosity of 2x10^{11} Msun per unit cluster mass evolves as (1+z)^{5.1+/-1.9}. These results assume a single star forming galaxy template; the presence of AGN, and an evolution in their relative contribution to the mid-IR galaxy emission, will alter the overall number counts per cluster and their rate of evolution. We infer the total SFR per unit cluster mass and find T_SFR/M_c ~ (1+z)^{5.4+/-1.9}. This evolution can be attributed entirely to the change in the in-falling field galaxy population. The T_SFR/M_c (binned over all redshift) decreases with increasing cluster mass with a slope (T_SFR/M_c ~ M_c^{-1.5+/-0.4}) consistent with the dependence of the stellar-to-total mass per unit cluster mass seen locally. The inferred star formation seen here could produce ~5-10% of the total stellar mass in massive clusters at z = 0. Finally, we show a clear decrease in the number of IR-bright galaxies per unit optical galaxy in the cluster cores, confirming star formation continues to avoid the highest density regions of the universe at z ~ 0.75 (the average redshift of the high-redshift clusters). While several previous studies appear to show enhanced star formation in high-redshift clusters relative to the field we note that these papers have not accounted for the overall increase in galaxy or dark matter density at the location of clusters. Once this is done, clusters at z ~ 0.75 have the same or less star formation per unit mass or galaxy as the field.

View original: http://arxiv.org/abs/1304.3335