2008/07/01 by Adam Muzzin, Gillian Wilson, Mark Lacy +2 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/591542
31 pages, 24 figures, 2 tables, accepted for publication in the ApJ. For version with high resolution figures see http://www.astro.yale.edu/amuzzin/papers/ms.pdf
arxiv created 2008/07/01 · openalex publication_date 2008/10/17 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
We present a catalog of 99 candidate clusters and groups of galaxies in the redshift range 0.1 < z phot < 1.3 discovered in the Spitzer FLS. The clusters are selected by their R c − 3.6 μ m galaxy color-magnitude relation using the cluster red-sequence algorithm. Using this cluster sample, we compute the 3.6, 4.5, 5.8, and 8.0 μ m cluster LFs. Similar to previous studies, we find that for the bands that trace stellar mass at these redshifts (3.6 and 4.5 μ m ) the evolution in M * is consistent with a passively evolving population of galaxies with a high formation redshift ( z f > 1.5). Using the 3.6 μ m LF as a proxy for stellar luminosity, we remove this component from the MIR (5.8 and 8.0 μ m ) cluster LFs and measure the LF of dusty star formation/AGNs in clusters. We find that at z < 0.4 the bright end of the cluster 8.0 μ m LF is well described by a composite population of quiescent galaxies and regular star-forming galaxies with a mix consistent with typical cluster blue fractions; however, at z > 0.4, an additional population of dusty starburst galaxies is required to properly model the 8.0 μ m LFs. Comparison to field studies at similar redshifts shows a strong differential evolution in the field and cluster 8.0 μ m LFs with redshift. At z ∼ 0.65 8.0 μ m -detected galaxies are more abundant in clusters compared to the field, but thereafter the number of 8.0 μ m 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 rapid differential evolution between the cluster and field LFs is qualitatively consistent with recent field galaxy studies that show that the star formation rates of galaxies in high-density environments are larger than those in low-density environments at higher redshift.