0 Assigned ID: 2695 ----- Attempting Submission 1 (Mon Jan 31 23:30:38 GMT 2022) ----- HST Phase I Proposal 2695 successfully submitted. Receipt: # 2695-1 ----- Attempting Submission 2 (Tue Feb 01 03:41:29 GMT 2022) ----- HST Phase I Proposal 2695 successfully submitted. Receipt: # 2695-2 ----- Attempting Submission 3 (Tue Feb 01 04:07:40 GMT 2022) ----- HST Phase I Proposal 2695 successfully submitted. Receipt: # 2695-3 0 ----- Attempting Submission 1 (Sun Mar 27 17:18:35 GMT 2022) ----- HST Phase II Proposal 16914 successfully submitted. Receipt: # 16914-1 ----- Attempting Submission 2 (Fri Apr 08 21:24:22 GMT 2022) ----- In the Belly of the Beast: Star Cluster Formation and Evolution in the Centers of local LIRGs We propose WFC3/UVIS F336W, F438W, and F814W observations for 8 Luminous Infrared Galaxies (LIRGs) in the Great Observatories All-Sky LIRG Survey (GOALS) scheduled for JWST Cycle 1 (GO1) observations. With a proprietary period of 0 days for 50% of the GO1 LIRGs, observations taken now will provide the concurrent WFC3/UVIS imaging necessary to reliably age-date the star clusters detected in these systems. In addition to our science goals these data will be made available for use by the community immediately, ensuring the maximum science return for the inaugural JWST Cycle. Recent HST observations provide evidence that the rate of cluster destruction in the nuclear regions of LIRGs is higher than that in their extranuclear regions, and higher than that observed in normal star-forming galaxies. The combination of HST and JWST NIRSPEC and MIRI IFU observations make possible a complete inventory of the properties of star clusters in the nuclear regions. The HST filters are needed to break the age-reddening degeneracy, and the JWST IFU observations will detect hydrogen recombination and PAH emission associated with the most embedded nuclear clusters. We will measure key properties such as the fraction of star formation residing in clusters, the nuclear and extranuclear cluster destruction rates, and the cluster formation efficiency. No telescopes other than the combination of HST and JWST are capable of obtaining the deep, high-resolution data required for such a multi-wavelength study of star clusters in LIRGs. HST images will be obtained using the WFC3/UVIS in imaging mode with the broad-band F336W filter as well as the broad-band F438W and F814W filters for two galaxies (NGC 5135 and ESO 420-G013). For the remaining 6 galaxies the new F336W observations will be paired with our pre-existing ACS/WFC F435W and F814W observations. The ACS/WFC and WFC3/UVIS cameras have comparable fields of view (202"x202" and 162"x162", respectively), and cover sufficient area to enable observations of these LIRGs in a single pointing. The clusters observed in this sample of LIRGs have M_V= -8 to -16 mag and apparent F435W (B) magnitudes typically in the range B ~ 21-25.5 mag. We have made use of instantaneous starburst models from Bruzual & Charlot (2003) to estimate the observed magnitudes in the F336W filter. For a 100 Myr starburst (F336W - F435W = -0.53 mag) and a conservative apparent magnitude of B=25.5 mag, we find that we can reach a signal-to-noise ratio, SNR, of approximately 10 with F336W, F438W, and F814W in roughly 2600, 1300, and 1300 seconds respectively. Note that if the clusters are younger, their spectral energy distributions peak even higher in bluer filters, and are therefore 1-2 magnitudes brighter than described above. Thus, in the absence of dust, the achieved SNR will be significantly higher. We model our observing strategy based on other studies of star clusters in luminous infrared galaxies (GO 14066 and GO 15472) and use a custom 4-pt dither pattern for each source designed to (1) remove the gap between the chips (1.2 arcsec) (2) sub-sample the PSF (half pixel or a third of a pixel shift have been included if the pattern is a multiple of 2 or 3, respectively), and (3) to remove droplets (shift of 4 arcsec required). The 4-pointing pattern has the following coordinates in arcsec: (0,0), (-3.69,1.31), (-2.5, -2.44), (1.19,-3.75). For the F438W we modify the WFC3-UVIS-GAP-LINE patten to include a third pointing at (0,0). For the F814W we adopt the standard WFC3-UVIS-GAP-LINE pattern. Thus the patterns are (0,0), (-0.092, -1.203), (0.092, 1.203) and (-0.089, -1.203), (0.089, 1.203) respectively. Further, the main body of the galaxy has been placed at the UVIS2-FIX location (which is more sensitive in the UV, and therefore, optimal to detect clusters), or at the UVIS-FIX location in order to fully map the galaxy if it has very extended tidal features. We use the latter aperture for VV340A, UGC5101, NGC5135, and Mrk 273. Finally, we observe in the ACCUM mode, and include a FLASH of 10 seconds with the CR_SPLIT=NO parameter to mitigate CTE losses. The data reduction and calibration of new and archival data will be done using the standard HST pipeline. IRAF, IDL and python will be used for additional data reduction and photometry within metric apertures. The cluster analysis will be done by using Source Extractor to identify clusters and IDL routines to extract aperture measurements of clusters and calculate luminosities. Similar analysis has been done on other F336W, F435W, and F814W datasets (Linden et al. 2017, 2021). Folding in the analysis data at other wavelengths from the Great Observatories All-Sky LIRG Survey (GOALS) will complete the interpretation of the HST dataset. This proposal is being submitted by members of the Great Observatories All-Sky LIRG Survey (GOALS: http://goals.ipac.caltech.edu) collaboration. The GOALS team has made extensive use of the Great Observatories and additional ground and space-based telescopes to conduct multi-wavelength investigations of luminous infrared galaxies (LIRGs). The team has published over 60 refereed papers, with about a third of them containing analysis of HST data. Specifically, Linden et al. (2017) and Linden et al. (2021) were studies of star cluster properties (ages, luminosity and mass functions, destruction rates) in a sample of GOALS galaxies imaged with the ACS/SBC (far-UV) and ACS/WFC (B and I-band) and WFC3/UVIS U, B, and I, respectively. Larson et al. (2020) was a study of Paschen-beta clump properties (size, luminosity, SFR) in a sample of GOALS galaxies imaged with WFC3 (F128N/F130N). Also of relevance to this proposal are the following ancillary datasets awarded to and analyzed by the GOALS team: HST ACS/WFC F435W and F814W observations of the high-luminosity end of the GOALS LIRG sample and Spitzer and Herschel mid- to far-IR imaging data. Nine members of the proposal team (Co-PI Dr. Linden, Dr. Armus, Dr. Diaz-Santos, Dr. Evans, Dr. Kim, Dr. Larson, Dr. Murphy, Dr. Rich, Dr. Surace) have extensive experience reducing and analyzing HST data. Further, half of the team has over a decade of experience studying star formation and AGN activity in LIRGs, and one members of the team (Song) is presently working on GOALS-related PhD thesis project. The Co-PIs of the submitted HST proposal are Evans and Linden. Dr. Evans leads the team at the University of Virginia, and he has PI'ed the majority of the GOALS broadband, UV-to-optical HST programs for the collaboration; the resulting papers have focussed on analyzing the structural properties of LIRGs and the properties of their optically-bright star clusters (which also includes data from PIDs 11196 and 15472: Evans PI). The UVA research teams taking primary roles on these publications includes Dr. Linden (now at UMASS Amherst), Dr. Kim and Dr. Privon, with Dr. Linden PI'ing the optical cluster property-related GOALS publications. The team working at Caltech, led by Dr. Armus, has led the HST near-IR and mid/far-IR Spitzer and Herschel investigations of line continuum emission from LIRGs, and is leading a JWST ERS program (ERS 1328, "A JWST Study of the Starburst-AGN Connection in Merging LIRGs") to study four lower luminosity infrared galaxies with NIRSpec, NIRCAM and MIRI. Overall, the Caltech research team taking primary roles on these near/mid-IR publications includes Dr. Howell, Dr. Mazzarella and Dr. Lai. Dr. Howell led the investigation of the GALEX and Spitzer (specific) star formation rates and global UV vs. IR properties of LIRGs. 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