Assigned ID: 476 ----- Attempting Submission 1 (Fri Feb 25 18:19:10 GMT 2011) ----- ----- Attempting Submission 1 (Fri Jun 17 19:21:24 GMT 2011) ----- Deep FUV Imaging of Cool Cores in Galaxy Clusters We propose to complete an on-going ACS/SBC FUV imaging survey of nearby galaxy cluster cores with the observation of our final 5 targets. This FUV program is the last critical element of a comprehensive investigation of the impact of stellar and AGN feedback on the local galaxy cluster environment. The HST images complement new, high-resolution, Halpha images obtained with the Maryland-Magellan Tunable Filter (MMTF) on the Baade 6.5m telescope, as well as new optical long-slit spectroscopy from the Magellan and Keck telescopes, Herschel mid-far IR imaging spectroscopy, CARMA, SMA and IRAM sub-mm imaging spectroscopy, and archival Chandra imaging spectroscopy, GALEX NUV imaging, and VLA 1.4 GHz maps. The MMTF data have revealed unsuspected filamentary complexes in several systems. The GALEX data often show hints of extended NUV and FUV emission on a similar scale, but their poor spatial resolution prevents meaningful comparison with the MMTF data. The ACS/SBC data which we acquired during the 2009 supplemental call have provided this much needed gain in resolution, but several of the most exciting Halpha filamentary complexes remain unobserved at FUV. The combined X-ray-FUV-Halpha-IR-radio imaging and X-ray-optical-IR spectra will allow us to derive with unprecedented precision the role of the AGN, hot stars, shocks, and relativistic particles on the excitation and thermodynamics of the multi-phase intracluster and interstellar media in these systems. This is an important question since the formation and evolution of most cluster galaxies have likely been affected by these processes.
Our objective is to obtain deep FUV images of 5 clusters that were missed due to the last HST service mission. The warm ionized H$\alpha$-emitting gas in all objects fits within a single SBC field of view. Thus, we choose a single pointing for all clusters in our sample -- yielding a total of 5 pointings. Following the words of advice from the ACS Instrument Handbook, we choose to observe each pointing through two different filters (F140LP \& F150LP) to ensure that the SBC ``red leak'' is properly removed and thus to properly isolate the true FUV flux. The well-known spatial shift between the F140LP and F150LP images will easily be corrected for during data reduction. Standard SBC ACCUM mode and small dither pattern will be used for the observations. 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