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We present a catalogue of 99 candidate clusters and groups of galaxies in theredshift range 0.1 < z_{phot} < 1.3 discovered in the Spitzer First Look Survey(FLS). The clusters are selected by their R - 3.6um galaxy color-magnituderelation using the cluster red sequence algorithm. Using this cluster sample wecompute the 3.6um, 4.5um, 5.8um, & 8.0um cluster luminosity functions (LFs).Similar to previous studies, we find that for the bands that trace stellar massat these redshifts (3.6um, 4.5um) the evolution in M* is consistent with apassively evolving population of galaxies with a high formation redshift (z_{f}> 1.5). Using the 3.6um LF as a proxy for stellar luminosity we remove thiscomponent from the MIR (5.8um & 8.0um) cluster LFs and measure the LF of dustystar formation/AGN in clusters. We find that at z < 0.4 the bright end of thecluster 8.0um LF is well-described by a composite population of quiescentgalaxies and regular star forming galaxies with a mix consistent with typicalcluster blue fractions; however, at z > 0.4, an additional population of dustystarburst galaxies is required to properly model the 8.0um LFs. Comparison tofield studies at similar redshifts shows a strong differential evolution in thefield and cluster 8.0um LFs with redshift. At z ~ 0.65 8.0um-detected galaxiesare more abundant in clusters compared to the field, but thereafter the numberof 8.0um sources in clusters declines with decreasing redshift and by z ~ 0.15,clusters are underdense relative to the field by a factor of ~5. The rapiddifferential evolution between the cluster and field LFs is qualitativelyconsistent with recent field galaxy studies that show the star formation ratesof galaxies in high density environments are larger than those in low densityenvironments at higher redshift.

astrophysical journal/the astrophysical journal

The Evolution of Dusty Star Formation and Stellar Mass Assembly in  Clusters: Results from the IRAC 3.6um, 4.5um, 5.8um and 8.0um Cluster  Luminosity Functions