Integrated H-alpha and Far Infrared Star Formation Rates of High Redshift Galaxy Clusters

Details Integrated H-alpha and Far Infrared Star Formation Rates of High Redshift Galaxy Clusters Integrated H-alpha and Far Infrared Star Formation Rates of High Redshift Galaxy Clusters

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sptz.prop20009f&link_type=abstract

Spitzer Proposal ID #20009

Computer Science

Scientific paper

We propose to study the evolution of star formation in galaxy cluster environments by pushing back measurements to the earliest epoch at which large samples of confirmed clusters exist, z ≃ 0.8. We will measure the integrated star-formation rates (SFRs) for 12 z ≃ 0.8 galaxy clusters using (1) MIPS 24 and 70 um photometry and (2) ground-based H-alpha imaging. Most importantly, the 12 z ≃ 0.8 clusters span the full range in mass, from near-group environment to the most massive cluster. The 6 highest mass clusters in the sample are targets of Spitzer GTO cluster programs (PIs: Rieke, Fazio). We request 18.6 hours to complete matching MIPS and IRAC imaging of 6 optically-selected, lower-mass clusters to provide an essential complement to the ongoing Spitzer GTO observations of massive clusters at this redshift. We have found that H-alpha-derived star-formation rates depend on both cluster mass and redshift. Therefore, one must sample the full range of cluster masses to reach robust conclusions regarding evolution. By observing 6 lower mass clusters, we will provide the key systematic test of any results obtained using the GTO targets. Our H-alpha imaging has better spatial resolution and is 3 times more sensitive in terms of SFRs than our proposed MIPS observations, which will detect galaxies with SFRs of 1 M_odot/yr. However, H-alpha imaging alone will miss heavily obscured star-forming galaxies that are commonly associated with interactions, and the interaction rate in clusters is expected to increase with redshift. The IRAC imaging will assist in source identification in the MIPS data and will provide robust stellar masses to quantify the total past star formation. All the lower mass clusters have extensive ancillary data, including HST imaging and ground-based imaging and spectroscopy. These data will allow us to study the morphology-density-SFR relation as well as compare [OII]/H-alpha/far-IR SFRs for several hundred cluster galaxies.

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