THE EVOLUTION OF DUSTY STAR FORMATION IN GALAXY CLUSTERS TO z = 1: SPITZER INFRARED OBSERVATIONS OF THE FIRST RED-SEQUENCE CLUSTER SURVEY

We present the results of an infrared (IR) study of high-redshift galaxy clusters with the MIPS camera on board the Spitzer Space Telescope. We have assembled a sample of 42 clusters from the Red-Sequence Cluster Survey-1 over the redshift range 0.3 < z < 1.0 and spanning an approximate range...

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Bibliographic Details
Published in:The Astronomical journal 2013-10, Vol.146 (4), p.1-13
Main Authors: Webb, T M A, O'Donnell, D, Yee, H K C, Gilbank, David, Coppin, Kristen, Ellingson, Erica, Faloon, Ashley, Geach, James E, Gladders, Mike, Noble, Allison, Muzzin, Adam, Wilson, Gillian, Yan, Renbin
Format: Article
Language:English
Subjects:
APPROXIMATIONS
ASTRONOMY
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CAMERAS
Clusters
Galactic clusters
GALAXIES
GALAXY CLUSTERS
GALAXY NUCLEI
Infrared
Infrared radiation
INTERMEDIATE INFRARED RADIATION
LUMINOSITY
MASS
NONLUMINOUS MATTER
RED SHIFT
STAR CLUSTERS
STAR EVOLUTION
Star formation
STARS
Statistical methods
Stellar evolution
TELESCOPES
UNIVERSE
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Summary:We present the results of an infrared (IR) study of high-redshift galaxy clusters with the MIPS camera on board the Spitzer Space Telescope. We have assembled a sample of 42 clusters from the Red-Sequence Cluster Survey-1 over the redshift range 0.3 < z < 1.0 and spanning an approximate range in mass of 10 super(14-15) M sub([middot in circle]). We statistically measure the number of IR-luminous galaxies in clusters above a fixed inferred IR luminosity of 2 x 10 super(11) M sub([middot in circle]), assuming a star forming galaxy template, per unit cluster mass and find it increases to higher redshift. These results are tied to the adoption of a single star forming galaxy template; the presence of active galactic nuclei, 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.
ISSN:0004-6256
1538-3881
1538-3881
DOI:10.1088/0004-6256/146/4/84