0 Assigned ID: 2564 ----- Attempting Submission 1 (Mon Sep 20 21:17:59 GMT 2021) ----- In this resubmission, I added FLASH=2 to the F475W and F814W exposures in visit 1 to get closer to the recommended level of 20 electrons for CTE mitigation. The F606W exposures already have an estimated background of 27.7 electrons, so no need to add FLASH there. The narrowband filter in visit 2 already had an appropriate level of FLASH specified. -- Max Mutchler 971579914 ----- Attempting Submission 1 (Wed Sep 29 16:04:15 GMT 2021) ----- ----- Attempting Submission 2 (Wed Oct 13 18:23:06 GMT 2021) ----- Imaging of Compact Cluster HCG 40 HCG 40, or Arp 321, is a compact galaxy group with 5 cluster members. Member galaxies include an optical AGN and galaxies at a variety of star formation rates as measured in both UV and IR, though no Hubble data on these objects yet exists. We propose to take broadband optical and H-alpha observations of HCG 40. We will obtain high signal-to-noise imaging of the compact galaxy group Arp 321, or HCG 40, with both broad and narrow band optical filters using the WFC3/UVIS instrument. No previous Hubble observations of this group exist. We propose to take new F475W, F606W, F814W, and F665N observations with WFC3/UVIS. The faintest and smallest member of HCG 40 has a total magnitude of R=15.4 and B=17.4, while the brightest and largest has a total magnitude of R=12.2 and B=13.8. Altogether, we request 6 orbits to make these observations. Using Arp 220 as a template spectrum in the WFC3/UVIS Exposure Time Calculator, we can achieve a S/N ratio of at least 100 per resolution element in F475W, F606W, and F814W with exposures of 2400s in F475W, 1000s in F606W, and 1100s in F814W, for the brightest cluster member, and at least 50 per resolution element in the faintest cluster member with 3600s in F814W. We can achieve high signal to noise for quality imaging by splitting 3 orbits between the broad-band filters. To highlight regions with high star formation activity, we request an additional 3 orbits with F665N on WFC3, which will reach high S/N in those areas and highlight the strong differences in star formation rate between cluster members. HCG 40 is at a redshift of z=0.0223, which still falls within the F665N filter's coverage. This filter is unavailable on ACS. The WFC3 field of view is also sufficient to encompass the entire cluster without constraint on orientation. We propose a single WFC3 pointing with a 3-point gap dither to mitigate artifacts such as cosmic rays, hot pixels, and the interchip gap. At the same time as the primary WFC3 observations, we will obtain parallel observations with ACS in F475W and F606W. The WFC3 dither shift is oversized a bit so that it also covers the ACS chip gap in the parallel field. With 3 orbits in each ACS filter we expect to detect many faint background galaxies in the parallel field. This target is schedulable in late 2021 at the desired orient. Scheduling as early as possible in November is ideal. The team has a wealth of experience in making outreach images for the Hubble Space Telescope and is responsible for creating Hubble images viewed by billions of people world-wide, including last year's 31st anniversary image which was viewed 1.4 billion times. The team includes decades of experience in writing Hubble news releases, designing informal educational and outreach products based on Hubble data, as well as instrument expertise specializing in treatment of WFC3 data. Galaxies 6 false SUPPORTED CLUSTER OF GALAXIES GROUP INTERACTING GALAXY TIDAL TAIL YES This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Magnitude is total for brightest cluster member, which also occupies roughly 30 square arcseconds. WFC3/UVIS Imaging No No F665N WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F606W WFC3/UVIS Imaging No No F814W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F475W POS-TARG DITHER 5 LINE false false 3 87 LINE 1 false The scheduling data was generated by CASM 29.2. 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