0 Assigned ID: 2189 ----- Attempting Submission 1 (Fri Apr 09 20:11:20 GMT 2021) ----- HST Phase I Proposal 2189 successfully submitted. Receipt: # 2189-1 ----- Attempting Submission 2 (Fri Apr 09 21:59:54 GMT 2021) ----- Added visit 14 as a duplicate to replace the failed visit 6. -1318490518 ----- Attempting Submission 1 (Mon Jul 26 18:35:01 GMT 2021) ----- ----- Attempting Submission 2 (Fri Oct 01 14:26:05 GMT 2021) ----- ----- Attempting Submission 3 (Wed Feb 15 17:24:13 GMT 2023) ----- I ignored the warning because APT was getting hung up trying to do the planners for previously completed observations. Intracluster Light in the Frontier Fields We propose a 20 orbit WFC3/IR campaign in the environs of HST Frontier Field (HFF) clusters to obtain the most comprehensive view to date of the intracluster stellar population and total baryon content in massive galaxy clusters. Our program builds upon the existing investment in the HFFs to provide contiguous coverage out to ~3 Mpc from the cluster center. We will use these data sets to make the first determination of the total stellar content, including the intracluster light (ICL), out to >0.65 r200 for each of the HFF clusters, directly constraining the extent to which the cluster galaxy population is altered by processes leading to ICL formation, and the radii over which these process are important. We will also compare the spatial distributions of the ICL, intracluster medium, galaxies, and dark matter within the central 300 kpc to establish whether the observed low scatter in the radial gas-to-stellar ratio masks underlying small scale variations due to various processeses such as ram pressure stripping, winds, and tidal stripping. This comparison will also test the recent assertion that the ICL is a highly robust tracer of the underlying mass distribution (based on work at smaller radii), and whether the ICL can be used by future missions such as Euclid and Roman to measure cluster mass distributions. Finally, we expect to be able to detect signatures of the splashback radius in at least some of these clusters, which we will use in conjunction with weak lensing masses to measure cluster mass accretion rates. Literature results for the HFF cluster MACS J1149.5+2223 demonstrate the feasibility of this program. Our proposed observations are designed to build upon the existing investment in the Frontier Fields to conduct a new, more complete census of the intracluster light (ICL) extending to large radii. The requested observations are constructed to span the gap between the primary and parallel BUFFALO survey fields. Geometry: The basic geometry for the proposed observations is two overlapping WFC3/IR frames bridging the gap between the primary and parallel BUFFALO fields. With proper overlap, the bridging fields can be used to correct for the temporal differences between the primary and parallel fields and enable continuous determination of the ICL brightness with radius. Two exposures is the minimum number required to have meaningful overlap between frames. In the phase 2 proposal we have included a constraint on the roll angle of +/-5 degrees from that of the BUFFALO fields to optimize the overlap with the BUFFALO fields and enhance the utility of the parallels; however, these can be relaxed as needed - in the proposal we stated that the core science can be achieved with an unconstrained roll angle. If the stated constraint is not possible, the second-best option would be a 180 degree rotation relative to the BUFFALO orient. The listed orient provides overlap of the ACS parallels with the core BUFFALO fields, mitigating edge effects for lensing and enabling greater coverge near the cluster core. A 180 degree rotation would place this overlap with the BUFFALO parallel fields instead. For MACS J0717.5+3745 and Abell 2744 there appear to be no schedulable visits with the preferred orient, so we have also included the 180 degree rotation in the plan explicitly as the second option. Filters: For this program, the science is driven by the need to extend spatial coverage in the WFC3/IR bands, both because of the smaller field-of-view of WFC3/IR and because the IR bands are most sensitive to intracluster light. The F105W and F160W filters provide a maximal wavelength lever arm in the IR bands for mapping out color gradients. Depth: The two requirements for the depth are that the data yield sufficient fidelity for the sky level determination, and sufficient sensitivity to enable a radial measurement of the ICL to ~2 Mpc. For the sensitivity, the observations benefit from averaging in annular bins extending over the width of the detector. From our experience with MACS J1149.5+2223, a single orbit in each filter provides sufficient S/N out to this radius. Special Requirements: All observations should be taken in LOW SKY (our depth calculations account for this). These conditions gain us 0.3 mag/arcsec^2 relative to the average sky, enabling us to increase the spatial extent over which we can resolve structure in the ICL. We request that the orientation of the WFC3/IR images be aligned with the BUFFALO survey WFC3/IR parallel observations to within 5 degrees. This orientation is designed to maximize overlap for relative sky calibration during LOW SKY conditions. Parallel Fields: To maximize the legacy value of this program and enhance the Frontier Fields data sets, we are taking parallel observations with ACS, split between F814W and F606W. These data will enable an extension of weak lensing analyses into these flanking regions. The PI for this proposal has been working on intracluster light for nearly two decades. He and his student have published a series of papers on the ICL (Gonzalez et al. 2001, 2005, 2007, 2013, 2021; DeMaio et al. 2015, 2018, 2020) spanning the redshift range z=0.1-1.75. The most recent of these papers (G21) demonstrated the feasibility of the current program by tracing the ICL to 2 Mpc for MACS J1149.5+2223 Zaritsky and Zabludoff have participated as co-authors in all of the above papers and have extensive expertise with low-surface brightness photometry. Montes is also an expert on the ICL, and was lead author on the paper demonstrating a correspondence between the dark matter and ICL distributions (Montes & Trujillo 2019). Jauzac also has experience with ICL in HFF clusters (e.g. Ellen et al 2019). She also has significant experience with the HFF clusters, is a leader of the BUFFALO survey, and more generally is an expert on lensing mass reconstructions. Cen also has broad expertise in cluster astrophysics. The PI, Zaritsky, Zabludoff, Montes, and Cen are also members of the BUFFALO survey. Deason is the lead author on the paper which identified the splashback radius signature in the ICL for the C-EAGLE simulations and brings her theoretical expertise to the program. Donahue is an expert on clusters and specifically the use of Chandra to constrain the properties of the ICM. She will contribute the Chandra maps for comparison with the ICL distribution. CoI Connor has generated photometric catalogs and photometric redshifts for the Frontier Field clusters, which will be used to help quantify the fraction of cluster luminosity contained in the ICL. CoI Koekemoer is an expert on construction of HST image mosaics, having led innovative techniques in numerous large HST programs since the early 2000s (incl GOODS, COSMOS, HUDF, CANDELS, CLASH, HFF, BUFFALO and others). He will produce HST mosaics for this program and participate in scientific work related to his interests in high-z galaxies and AGN. Large Scale Structure of the Universe Galaxies 6 false false false false false false false SUPPORTED CLUSTER OF GALAXIES RICH CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 CLUSTER OF GALAXIES RICH CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 CLUSTER OF GALAXIES RICH CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 CLUSTER OF GALAXIES RICH CLUSTER J2000 J2000 CLUSTER OF GALAXIES RICH CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 CLUSTER OF GALAXIES RICH CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 CLUSTER OF GALAXIES RICH CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 CLUSTER OF GALAXIES RICH CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 CLUSTER OF GALAXIES RICH CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 CLUSTER OF GALAXIES RICH CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/IR Imaging No No F105W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F105W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F105W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F105W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F105W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F105W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F105W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F105W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F105W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F105W WFC3/IR Imaging No No F160W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W The scheduling data was generated by CASM 29.2. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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