Tracing star cluster motions from their birth to dispersal in the barred spiral galaxy M83

submission 3 1335139423 Assigned ID: 4993 ----- Attempting Submission 1 (Mon Mar 18 12:34:43 GMT 2024) ----- HST Phase I Proposal 4993 successfully submitted. Receipt: # 4993-1 ----- Attempting Submission 2 (Mon Mar 25 21:10:51 GMT 2024) ----- HST Phase I Proposal 4993 successfully submitted. Receipt: # 4993-2 ----- Attempting Submission 3 (Tue Mar 26 20:04:12 GMT 2024) ----- HST Phase I Proposal 4993 successfully submitted. Receipt: # 4993-3 ----- Attempting Submission 4 (Tue Mar 26 22:57:30 GMT 2024) ----- HST Phase I Proposal 4993 successfully submitted. Receipt: # 4993-4 ----- Attempting Submission 5 (Wed Mar 27 00:01:05 GMT 2024) ----- Repeat two failed and approved exposures. -1590823784 ----- Attempting Submission 1 (Tue Aug 13 20:30:06 GMT 2024) ----- ----- Attempting Submission 2 (Mon Oct 07 18:08:33 GMT 2024) ----- ----- Attempting Submission 3 (Wed Jan 29 02:51:51 GMT 2025) ----- ----- Attempting Submission 4 (Thu Feb 19 15:33:01 GMT 2026) ----- This is a repeat of failed exposures. FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser 0 Tracing star cluster motions from their birth to dispersal in the barred spiral galaxy M83 We propose to image the nearby barred spiral galaxy M83 with WFC3 in NUV (F275W; 3x3 tile). The new NUV imaging, in conjunction with the substantial archival coverage in multi-bands (U, B, V, I & Halpha), is an established tool to accurately measure star cluster ages and masses by overcoming the age-extinction degeneracy. In addition, new ALMA CO(1-0) data of the full galactic disk detected 5,724 molecular clouds to their lowest mass of 10^4Msun, and set a stage for substantial statistical analyses at every subregion within the disk. Combined with this largest and most complete cloud catalog in any external galaxy, the cluster distribution, and their spread with age, will reveal the emergence of star clusters in molecular clouds -- where and which molecular clouds can form clusters, what the cloud-cluster mass relation is, whether young clusters disperse their parental clouds or they simply drift away from the clouds, and how they disperse and merge into large-scale galactic structures and dynamics. The last point will be analyzed in relation to the debate on the origin of spiral arms --whether spiral arms are steady, long-lived structures supported by the classic density-wave theory, or transient, short-lived structures continuously generated and dispersed by swing amplification. Primary WFC3: by adding mosaic imaging in F275W, this project aims to complete the HST/WFC3 multi-band photometric coverage of the closest, prototypical barred spiral galaxy M83. The proposed area (see Fig 1 yellow box) is covered by the archival data in F336W, F438W, F547M/F555W & F814W (see Fig 2 top). We aim to add F275W for the whole area (3x3 mosaic tiles, 1 visit per tile, 9 visits in total). Because of the irregular shape of the archival coverage, observing exactly the same area in F275W puts significant constraints in scheduling. We therefore request for a simple 3x3-tile for F275W, which covers a slightly larger area with some flexibility in scheduling. Each orbit consists of 4-point dither and provides 2105s exposure per pointing position. Parallel ACS: M83 has an extended ultraviolet (XUV) disk outside the traditional optical disk (Thilker et al. 2005; Bigiel et al. 2010). Parallel ACS observations can cover some part of the XUV disk (Fig 5). The parallel ACS could be taken at any orientation, but the southern part (as shown in Figure 5) has more UV blobs and is scientifically most optimal. We will use F475W and F814W filters in each orbit. For the 4-point dither pattern, we follow the recommendation in the report by Jay Anderson and Norman Grogin "Dithering for ACS and WFC3 Primes and Parallels" (issued Oct 18, 2023). We fiddled the exposure time at each dither position to minimize the overheads in both Primary and Parallel observations. In each visit (mosaic tile), the current setup provides 305, 700, 750, and 350 sec exposures in F275W (Primary), and 225 and 670 sec in F814W (Parallel) and 670 and 340 sec in F475W (Parallel). Angela Adamo, is an expert of star cluster identification and analysis with HST and JWST data. Daniela Calzetti, is an expert on star formation and dust obscuration. She has extensive experience with HST imaging data, and both stellar population and dust modeling. She has modeled spectral energy distributions of both whole star-forming galaxies and clusters within galaxies. She has been/is the PI of multiple HST programs, including the Cycle 21 Treasury project LEGUS (Legacy ExtraGalactic UV Survey). David Thilker, is an expert of nearby galaxies, the evoluton of stellar systems, optical and radio astronomy. He developed the PHANGS-HST cluster identification pipeline. This project will utilize this pipeline. Fumi Egusa, is an expert of mm-wave and infrared astronomy, gas and stellar dynamics around spiral arms in disk galaxies. She is one of the first who used the relative distribution of gas and stars to trace spiral arm dynamics - the technique that the proposed project plans to use. Akihiko Hirota, is an expert on mm-wave astronomy, molecular gas dynamics and star formation in nearby galaxies. His analysis of molecular clouds in the ALMA CO(1-0) data will form a critical anchor for the proposed study of star cluster dispersal from the prominent molecular structures. Jin Koda, has substantial experience in optical and mm-wave asttronomy and numerical simulations of galactic disks. He has publications on analyses of galactic properties, stellar populations, star formation in galaxies with optical data. He is also an expert on molecular clouds and star formation in nearby galaxies. He also developed an N-body/SPH code and has publications in galaxy formation simulations as the PI. Galaxies Stellar Populations and the Interstellar Medium 6 false true false false false false false SUPPORTED GALAXY DISK SPIRAL SPIRAL ARM J2000 J2000 WFC3/UVIS Imaging No No F275W ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F814W 1738118905037 Hst Same orient constraint links visits (19 20 21 22 23 24 25 26 27) The scheduling data was generated by CASM 32.1.3. 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