Star formation in the Infall Regions of Intermediate Redshift Clusters

Details Star formation in the Infall Regions of Intermediate Redshift Clusters Star formation in the Infall Regions of Intermediate Redshift Clusters

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50733r&link_type=abstract

Spitzer Proposal ID #50733

Computer Science

Scientific paper

There are well known correlations between star formation and environment such that clusters have a much lower fraction of star forming galaxies than groups or the field. Clusters may therefore play an important role in supressing star formation in galaxies. Local studies have supported this scenario but have not been able to isolate the mechanisms that suppress star formation since the majority of galaxies in clusters have already ceased forming stars. To determine how clusters transform galaxies en masse it is necessary to catch the transformation 'in the act'. We propose panoramic MIPS 24 micron imaging of 7 well studied galaxy clusters at 0.55 < z < 0.8 drawn from the ESO Distant Cluster Survey (EDisCS). We will measure how the fraction of star forming galaxies depends on local galaxy density and on clustercentric distance, probing with one data set from the cluster cores, through the infall regions, and into the field. The requirements of this survey are influenced by our experience from EDisCS. It must have 1) observations at large lookback times when the galaxy population in clusters was rapidly evolving, 2) a large sample of clusters with a large range in velocity dispersion to determine the dependence of star forming galaxy fraction on cluster mass, 3) measurements to large clustercentric radii to probe local densities comparable to groups but in the vicinity of clusters, and 4) data at MIR wavelengths to measure SFR unbiased by dust obscuration. Our EDisCS clusters are the best studied systems at these redshifts, with optical and near infrared ground-based imaging, HST imaging, extensive deep VLT spectropscopy, XMM-Newton data, and deep IRAC and MIPS data, all on the central ~2.5 x 2.5 Mpc of each cluster. Most importantly, they are part of an extensive wide--field spectroscopy program covering ~12Mpc x 12Mpc, which will yield unambiguous cluster membership and determinations of the local environment.

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