In this revision, we convert the subarray U exposures to have the exact same full-frame and extended gap dither pointings as the other two filters. - Max Mutchler ----- Attempting Submission 3 (Thu Aug 02 16:50:45 GMT 2012) ----- We propose to image the host galaxy and surrounding cluster of the powerful radio galaxy Hercules A. The observations will be used to (1) study the colors and morphologies of the cluster members and to look for interactions with the extended radio lobes, (2) investigate the nature of the obscuring rings in the host galaxy, and (3) create a visually appealing color image to be used in a press release with new very deep EVLA observations. We want wide filters (for S/N) which avoid bright emission lines (so as to give stellar con- tinuum only to allow interpretation of the colors). The optical spectrum by Buttiglioni et al 2009 shows the [OII] 3727 and H-alpha+[NII] lines are bright, the [OI] 6300 line is moderate, and the [OIII] 5007 line is faint (and likely to be confined to the nucleus). So the wavelength range between [OII] and [OI] in the observers frame 4300-7270 is available. The F606W filter fits in this range and has a high throughput. F625W also fits but has smaller bandwidth so will be somewhat less sensitive. The F336W filter fits blue-ward of [OII] and gives a long baseline in wavelength for measuring galaxy colors and obscuration in the rings. The broad red filter F814W will allow the spectral energy distribution (SED) of the stellar pop- ulations to be determined. To calculate exposure times we consider A1689, a well studied Abell cluster at similar redshift (z=0.183). The faint end of the galaxy luminosity function is at V=24 (Wilson etal. 1997). This can be reached in one orbit each with the F606W and F814W filters. In one orbit the F336W (U) filter will provide good detections of cluster ellipticals down to V=21, and deeper for any galaxies which are star forming, and will allow a measure of the optical depth of the obscuring rings. The observations in each filter should be dithered to allow removal of hot pixels, cosmic rays, and the chip gap. AGN/QUASARS 0 false 0.0 0.0 false false false false SUPPORTED GALAXY LOBE This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 WFC3/UVIS Imaging No No F606W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F814W POS-TARG MOSAIC DITHER 2 40 LINE false true 1.0 2 90 POS-TARG LINE 45 1 true The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. /private/var/folders/p2/p2FzDectHHyDUTVHYrBDpE++4r+/-Tmp-/OPVisit2131452192041094006.xml 1343925299342 (Tic-Visit :proposal-id 13065 :visit-id "01" :proposal-version -1 :trans-version "20120604" :date "02-Aug-2012 12:34:59.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 3464976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13065 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13065 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2896 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3229 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13065 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2782 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3229 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13065 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3006 :al-overhead-at-end 116 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3229 :pcs-gap 0 ) true 3 0