Other
Scientific paper
Mar 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50292m&link_type=abstract
Spitzer Proposal ID #50292
Other
Scientific paper
We propose deep, wide-field IRAC/MIPS 24um and 70um observations of one of the richest, developing filamentary-type clusters in the nearby universe for the purpose for measuring galaxy activity (AGN/star-formation;SF) down to M*+3 with SF rates >1M_solar/yr. Given the rapid progression of ``downsizing'' since z<1, one would expect to see most of the activity in the lower mass population. Abell 1882 at z~0.14 has one of the most diverse environments of any filament-type cluster previously studied and is made up of high density groups which are interconnected via X-ray filaments. This cluster is a system in formation undergoing a phase of mass accretion and has a large and active radio population (45 with measured z's - with photo-z 100) whose radio power source is unknown. The region of interest is matched by our coverage at other wavelengths (radio, optical, NIR, UV). Past Spitzer 24um studies have demonstrated the prevalence of dust-obscured active populations in higher redshift structures (clusters, superclusters). Their 24um data along with other wavelengths have pointed to obscured activity which was assumed to be SF. The potential error in translating 24um to SFR is huge if one does not know the MIR/FIR SED or even whether the sources might be AGN! We will use 24 and 70um to calculate the best fitting SED (hence derive accurate FIR, 5x better) which will then allow us to calculate the q=log(FIR/radio) value, taking into account the cold dust temperature. A factor of 5x improvement in FIR is well-matched to q studies. It is the difference between a q=1.60 and q=2.30 galaxy, where q=1.60 is used as a dividing line between an AGN & SF. The key questions we will answer are: Is there a correlation between SB and AGN activity and the galaxy density, and if so on what spatial scales? Is there a systematic difference between the SB and AGN activity, as a function of local galaxy density and X-ray brightness?
Arnouts Stephane
Dickinson Mark
Frayer David
Keel William
Miller Chris
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