0 Assigned ID: 390 ----- Attempting Submission 1 (Fri Apr 05 10:25:50 GMT 2019) ----- HST Phase I Proposal 390 (Tadpoles_v10.apt) successfully submitted. Receipt: # 390-1 ----- Attempting Submission 2 (Fri Apr 05 13:14:31 GMT 2019) ----- HST Phase I Proposal 390 (Tadpoles_v11.apt) successfully submitted. Receipt: # 390-2 ----- Attempting Submission 3 (Fri Apr 05 18:40:38 GMT 2019) ----- Improvements to ACS visits as per recommendations by the ACS reviewer: 1) switched 3 point to 4 point dither. 2) Visit 7 slightly decreased orient range to avoid bright star causing potential ghosting. 904638829 ----- Attempting Submission 1 (Fri Jul 05 19:49:15 GMT 2019) ----- ----- Attempting Submission 2 (Thu Jul 25 21:00:27 GMT 2019) ----- ----- Attempting Submission 3 (Tue Aug 27 21:58:41 GMT 2019) ----- Accretion-Triggered Starbursts in Tadpole Galaxies Gas accretion onto galaxies is believed to drive the average star formation rate. However, there are few observations of this accretion for late-type galaxies, especially impacting the disk or triggering a starburst in the disk. Here we propose optical and Halpha imaging of four metal-poor tadpole galaxies that have local metallicity drops by a factor of ~5 in relatively large off-center starburst clumps. The bursts and the unusual metallicities suggest recent accretion of large gas masses. Photometry plus SED modeling will determine the ages, masses, and luminosity distributions of the star clusters and star complexes in the bursts. Halpha will reveal ionization rates along with feedback and possible accretion structures. The sample represents the nearest low-mass galaxies that have high-resolution metallicity variations and single dominant starburst clumps. The results have broad implications for understanding the mass-metallicity relation for galaxies, the formation and feedback of stars and massive clusters in accretion-induced starbursts, and the origin of metal-poor globular clusters in the early universe. Only HST has the combination of angular resolution and sensitivity to carry out this program. We are imaging 4 tadpole galaxies with 3 NUV to optical filters and 1 H-alpha filter for 4 orbits each for a total of 16 orbits. These galaxies have a clear metallicity drop measured in the head vs. the tail with a clear star-forming head and an extended tail. The F390W filter samples the rest-frame NUV redward of the 2175A dust 'bump'. F547M samples the optical red- ward of the [OII] 3727 A line and the Balmer break at 3650A and is blue-ward of H-alpha making it perfect for continuum subtraction. F814W samples the red-optical. F657N samples the H-alpha line and is broader than F656N to encompass possible blueshifts or redshifts with respect to the galaxies. We are obtaining 3 dithered exposures per filter to clean them of cosmic rays and image artifcats and subsample the PSF. We use a 3 point dither pattern with the step sized multiplied by a factor of 5 for WFC3 to dither over the blotchy pattern remaining in the background of the observations. We use a 4 point dither pattern with a step sized multiplied by 17 for ACS. We post-flash F390W by 5e-, F547M by 2e-, and F657N by 9 e- to get to 12e- background per exposure. We use WFC3/UVIS for the blue filters and F657N, and use ACS/WFC for F814W since it has approximately a factor of 2 higher throughput in the red. We use F657N with WFC3/UVIS instead of ACS as it is broader than the H-alpha filter on ACS allowing us to include possible blue or redshifted flux. We will drizzle all images to the same plate scale for pixel-matched images. We place the entire galaxy on one chip as not to have the chip gap on the galaxy. We place the galaxies on Chip 2 of WFC3 as it has a slightly higher throughput in the UV. We place the galaxies on Chip 1 of ACS as it has lower read noise. We place the galaxy on the center of the chip aligned with the chip to capture peripheral emission. We ensure that the head to tail direction is not in line with the readout direction. We make sure the allowed PAs are sufficiently wide for easy scheduling. Our team has the necessary technical and scientific expertise to undertake all the investigations discussed in this proposal. PI Bruce Elmegreen was PI on the previous proposal for Kiso 5639 which was published promptly after the observation. He is an expert on star formation and the formation of massive clusters, and on the use of Halpha to determine the properties of nebular and star formation feedback. Co-I Debra Emegreen is an expert on photometry and morphology of galaxies. Co-I Marc Rafelski is an expert at obtaining, reducing, and analyzing WFC3 and ACS data and has experience measuring the photometry and morphology of galaxies. Co-I Morton Andersen is an expert on stellar systems and observational techniques. Co-I Jorge Sanchez Almeida is an expert on measuring metallicities, on the mass-metallicity relation, on extremely low metallicity galaxies and BCD galaxies, and on the kinematics of galaxies. Co-I Casiana Munoz-Tunon is an expert on giant star forming regions and BCD galaxies, and on tadpole galaxies. Co-I John Gallagher is an expert on star formation and stellar systems, on observational techniques, and on massive star clusters. 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