First submission -540248356 Assigned ID: 3204 ----- Attempting Submission 1 (Fri Mar 25 12:19:11 GMT 2022) ----- For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. First Phase II submission. 329787479 ----- Attempting Submission 1 (Tue Jun 28 19:58:39 GMT 2022) ----- The warning is regarding FP-POS=all. For G130M/1291 the available FP-POS are 3-4 for LP5. Both of which are used on all the visits. What's hidding in the neutral gas? Dissecting the different metallicity components in NGC 1313 Metallicity is a critical parameter shaping the evolution of galaxies on cosmic timescales. In spite of the importance of this single parameter and the variety of tools available to investigate its distribution in star-forming galaxies, detailed comparisons of the abundances obtained from the ionized-gas, neutral-gas, and stellar components are still lacking to fully understand the chemical state and evolution of galaxies. We propose to remedy the situation by exploiting the unique capabilities of HST/COS in the FUV regime, acquiring and analyzing G130M/1291 spectroscopic observations of 7 pointings (2 archival + 5 new) in the low-metallicity environment of NGC 1313. The data will provide a rich assortment of neutral-gas metallicity tracers allowing us to assess the abundances of the neutral ISM and estimate the stellar metallicities of the targeted stellar clusters. Our study will combine the metallicities of the neutral gas and stellar populations with existing abundances of the ionized gas, performing the first co-spatial comparison of these three components in a low metallicity system, investigating the degree of homogeneity between the stars and multi-phase ISM across the galaxy on spatial scales of ~55 pc. This complete and inexpensive study in the barred spiral NGC 1313 will uncover the links between the different internal components (stars, neutral and ionized gas), and their precise roles in moderating the mixing timescales and star formation in galaxies. This HST/COS program observes 5 young massive clusters (YMCs) in the nearby barred spiral galaxy NGC 1313 with the G130M/1291 COS configuration in 5 different visits. Each individual visit acquires the target using the ACQ/IMAGE mode with MIRRORA. The spectroscopic observations are collected using FP-POS = 3 and 4. Target Selection: At a distance of ~4.4 Mpc, NGC 1313 is an ideal target for a spatially-resolved study with the 2.5" COS aperture, as it allows us to sample the abundances of stellar clusters and the warm ISM on spatial scales of ~55 pc. This COS sample of YMCs covers a broad parameter space both in stellar ages (1-20 Myr) and spatial scales (R~ 0.1-4.4 kpc). The broad range in stellar ages is essential to test mixing timescale scenarios in a lower metallicity regime, particularly those where newly-synthesized metals take more than ~10 Myr to fully mix on spatial scales of <~100 pc. The exposure times were calculated assuming the spectrum of a simple stellar population of age 5 or 25 Myr (based on photometric ages) renormalized to the WFC3/F275W magnitudes to reach S/N~10 at 1250 A. The members of our team are experts in the field of UV spectroscopy (Dr. Hernandez, Dr. James, Dr. Aloisi, Dr. Mingozzi, Dr. Hirschauer, Dr. Jones and Dr. Adamo). Dr. Hernandez, Dr. James, Dr. Aloisi, Dr. Smith, Dr. Jones and Dr. Adamo have ample experience with HST/COS spectroscopy in particular. They have lead several HST/COS observing and archival campaigns to study the environments of nearby star-forming galaxies. Dr. James (deputy manager of the COS team) and Dr. Hirschauer are current members of the COS instrument team at STScI. Dr. Aloisi was the COS team lead 2006-2013. Dr. Hernandez was a research and instrument analyist for the same team from 2012-2014. Their years of service has equipped them with ample experience with the COS intrument, and its capabilities. Dr. Hernandez, Dr. James, Dr. Jones and Dr. Aloisi are experts in determining chemical abundances (of the stars and gas) from FUV spectra and photoionization modelling of HII regions. Dr. Smith is an expert in the characterization of young stellar populations, particularly massive stars. Dr. Hirschauer is an expert in both COS observations and star-forming region abundances as it pertains to dwarf galaxies, dust and the mechanisms that facilitate star formation. Dr. Aloisi, Dr. Smith and Dr. Adamo are experts in the field of star formation and stellar populations in nearby galaxies. Dr. Faucher-Giguere is an expert in large-scale numerical simulations and analytic modeling and a member of the FIRE (Feedback In Realistic Environments) collaboration. Stellar Populations and the Interstellar Medium 6 false false true false false false false SUPPORTED STELLAR CLUSTER YOUNG ASSOCIATION NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 F275W =17.3 STELLAR CLUSTER YOUNG ASSOCIATION NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 F275W = 16.3 STELLAR CLUSTER YOUNG ASSOCIATION NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 F275W = 17 STELLAR CLUSTER YOUNG ASSOCIATION NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 F275W = 17.4 STELLAR CLUSTER YOUNG ASSOCIATION NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 F275W = 16.5 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 30.3. 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