0 Assigned ID: 223 ----- Attempting Submission 1 (Thu Apr 04 17:12:25 GMT 2019) ----- HST Phase I Proposal 223 (MUDF_F336W.apt) successfully submitted. Receipt: # 223-1 ----- Attempting Submission 2 (Fri Apr 05 08:22:31 GMT 2019) ----- HST Phase I Proposal 223 (MUDF_F336W.apt) successfully submitted. Receipt: # 223-2 ----- Attempting Submission 3 (Fri Apr 05 15:53:59 GMT 2019) ----- HST Phase I Proposal 223 (MUDF_F336W.apt) successfully submitted. Receipt: # 223-3 0 ----- Attempting Submission 1 (Tue Jul 09 17:07:27 GMT 2019) ----- We propose an 8 orbit WFC3/UVIS F336W imaging program in the MUSE Ultra Deep Field to obtain a deep view of galaxy star formation histories and morphologies at the peak and decline of cosmic star formation (z<2.5). Our program is made unique by two main factors. First, this proposal is built upon the synergy of two public observational programs in this field, a MUSE survey and the deepest HST grism survey with the WFC3/G141 grism. Second, the choice of the field, which hosts several rich galaxy groups at z=0.7-1.1 and two quasars separated by less than 500 kpc at z=3.2. The quasars act as light beacons to probe the gas in and around the group galaxies, making this field ideal for studies of the interaction of galaxies with their local environment. Taking advantage of the unrivaled HST capabilities in the UV, we aim to observe galaxies transitioning from the star forming main sequence to a passive population. Our goals are twofold. i) We will accurately quantify the recent star formation histories of the galaxies and their dust content, which, when complemented by the gas budget, will unveil the physical processes responsible for the onset of a population of passive objects down to 10^9 Msun in stellar mass. ii) We will study the morphology of the young stellar populations probed by the rest-frame far-UV images, which compared to the morphologies of the bulk of the stellar emission and of the nebular emission maps (from the WFC3/IR program), will yield a resolved view of the quenching events. This proposal enables new science goals in this unique field, greatly increasing its legacy value for the astrophysical community. This program images the MUSE+HST Ultra Deep Field with the WFC3/UVIS F336W filter to obtain rest-frame UV imaging data. Full orbit integrations are obtained in order to minimize post-flash and read-noise and maximize the total depth. Therefore 4 orbit vists are required to enable fully cleaning the cosmic rays (as described in our phase I). Exposures are post-flashed by 4e- to help mitigate the CTE, and reach 12e- backgrounds per pixel. The dither pattern per visit is set 19 times larger than the default box pattern to help minimize the blotchy pattern observed in F336W imaging (i.e., similar to that seen in Rafelski et al. 2015, AJ, 150 31, Figure 15) and to dither over the chip gap to ensure a minimum of 7 exposures covering the entire field. As discussed in our phase I, we require an orient that is ~0, 90, or 180 degrees from whatever orient the first visit executes at to maximize our overlap of the two visits, as non-overlap regions will not have enough exposures to fully clean the cosmic rays from orbit long exposures. Therefore, the second visit is set to within 10 degrees of a 90 degree rotation. Also as described in the Phase I, to maximise the scientific return of this data in combination with the MUSE and WFC3/IR data we wish to observe this target within 1 year of the completion of the WFC3/IR observations (PID: 15673) which is currently foreseen for September 2019. Our program is not significantly affected by the possibility of one gyro mode. If we were to go into one gyro mode, it may affect the schedulability of the second orientation. We could accept the same orient or 180 degree rotation instead of the 90 degree rotation we are currently using. Note: if we did switch orients, we would need to add an offset for the second visit to maximize the dither pattern usefullness. Our team has the necessary technical and scientific expertise to undertake all the investigations discussed in this proposal. PI Fossati is an expert in the study of star formation in galaxies and has developed codes to analyze spectroscopic and imaging datasets to reconstruct the star formation history of galaxies. Co-I Rafelski is involved in several WFC3 projects, he has extensive experience in the analysis of WFC3 grism and imaging data and has scientific expertise on studying the gas in and around galaxies. He is also the co-PI of the WFC grism survey in the P2139-443 field. Co-I Fumagalli is the PI of the MUSE Ultra Deep Field and has extensive experience in the analysis of MUSE data and WFC3 UV imaging. Co-PI Fumagalli, Co-I Peroux, Morris and Bielby have scientific expertise in the study of the CGM combining high-resolution spectroscopy with IFU and MOS redshift surveys. Co-I D'Odorico is the PI of the ESO/UVES programme in the P2139-443 field, and she has extensive expertise in the analysis of the high-resolution spectroscopic data. Co-I Pirzkal is highly experienced in the analysis and exploitation of the WFC3 grism data, including the analysis of FIGS, PEARS, and GRAPES surveys. He is also the author of the EM2D method for reconstructing 1D spectra from multiple ORIENTs. Co-Is Papovich, Estrada-Carpenter, Lofthouse, Prichard, Revalski, and Dayal are experts on galaxy evolution, including modelling galaxy properties and measures of galaxy environments. CoI Lusso has expertise in the physics of quasars in connection to their environment. CoI Theuns is a core member of the EAGLE project and is an expert in the study of IGM and galaxy evolution with cosmological simulations. Co-I Arrigoni Battaia is an expert in the study of extended nebulae associated with quasars. 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