0 Assigned ID: 3573 ----- Attempting Submission 1 (Fri Mar 25 21:19:57 GMT 2022) ----- HST Phase I Proposal 3573 successfully submitted. Receipt: # 3573-1 ----- Attempting Submission 2 (Fri Mar 25 22:19:35 GMT 2022) ----- In this submission we include a request that the orientations for visits 2-4 be the same as visit 1 (to maximize field overlap and coverage of WFC3 chip gaps). 1461725991 ----- Attempting Submission 1 (Thu Jul 14 18:58:31 GMT 2022) ----- Taming the BEAST of N66 to resolve how star formation shapes the interstellar medium at low metallicity Although galaxies evolve by assembling the interstellar medium (ISM) into stars, standard gas tracers fail to account for the total ISM mass available for star formation. This is especially true at low metallicity and in strong radiation fields where dust shielding and dense molecular gas are scarce. Dust provides an independent tracer across phases, but its basic properties -- mass, grain size and extinction curve -- are poorly constrained between diverse environments. We propose to survey N66, the largest star-forming region in the low-metallicity Small Magellanic Cloud (SMC) with optical and ultraviolet imaging from Wide Field Camera 3. Along with archival imaging in the optical and IR from HST and JWST, we will constrain the intrinsic properties of resolved stars and the intervening dust independently from systematics of IR emission surveys and at 10x higher resolution. We will (1) quantify the influence of ionizing radiation fields on fundamental dust properties (2) map the ISM mass independently of emission systematics to quantify the nature of ``dark" gas at low metallicity. HST is the only observatory with the superb resolution and UV sensitivity necessary for these objectives, and N66 is the perfect laboratory for quantifying the influence of star formation activity on the structure of the ISM in the SMC, an excellent prototype for galaxies in the distant Universe. In this program we plan to obtain WFC3/UVIS imaging in four bands: F225W, F275W, F336W and F475W. We design our pointing to replicate archival F555W and F814W observations (PIDs 10248, 13680) and to cover the extent of the ISM structure of interest (4 pointings required). For each pointing, we arrange the exposures to minimize overheads. We include multiple exposures per band in order to include dither patterns (4 exposures each in F225W, F275W and F336W, and 3 exposures in F475W). In addition, we include a short ``guard" exposure in F475W (5s) to capture bright sources. Team: Claire Murray, Yumi Choi, Karl Gordon, Karin Sandstrom, Ben Williams, Julia Roman-Duval, Caroline Bot, Karoline Gilbert, L. Cliff Johnson, Roger Cohen, Petia Yanchulova Merica-Jones, Martha Boyer, Alec Hirschauer, Kristen McQuinn, Christina Lindberg PI Murray is an expert in the multiphase interstellar medium traced by radio spectral lines and resolved stellar populations. As the PI of Scylla, a 500-orbit HST imaging program (PIDs 15891, 16235, 16786) in parallel with ULLYSES to survey dust in the Magellanic Clouds, Murray has extensive experience with planning, executing and analyzing multi-wavelength resolved stellar photometry from HST. PI Murray will lead the observations, and oversee data reduction and analysis. Co-I WIlliams will lead the data reduction effort, including photometry and artificial star tests required for quantifying uncertainty, completeness and bias. Co-I Williams has a full decade of experience with these tasks for virtually all multi-wavelength HST surveys of resolved stellar populations in the Local Group, including PHAT, PHATTER, SMIDGE, METAL and Scylla (PIDs 12581, 13659, 14675, 15891, 16235, 16786). The team includes experts on the gas (Murray, Roman-Duval), dust (Gordon, Sandstrom, Bot, Johnson, Hirschauer), ISM structure (Yanchulova Merica-Jones, Lindberg), and stellar populations (Gilbert, Williams, Boyer, Cohen, McQuinn) of galaxies in the Local Group. This includes science analysis (star formation histories, rare stellar types, star formation feedback, dust production and destruction) as well as technical execution of HST observations. All of the team members are part of the Scylla survey, which will provide excellent comparison for this study. 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