Official Submission 205400993 Assigned ID: 3515 ----- Attempting Submission 1 (Fri Mar 25 20:37:21 GMT 2022) ----- HST Phase I Proposal 3515 successfully submitted. Receipt: # 3515-1 ----- Attempting Submission 2 (Tue Mar 29 19:47:20 GMT 2022) ----- COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. 0 ----- Attempting Submission 1 (Thu Jul 14 14:04:17 GMT 2022) ----- I am aware of the calibration limitations of extended sources. While oxygen and nitrogen have been widely observed in spiral and dwarf galaxies, the study of the next most abundant element, carbon, remains relatively unexplored, especially for the lowest metallicities relevant for high-z galaxies. Carbon has no strong collisionally-excited emission lines in the optical, however, by observing the CIII] 1907,1909 and OIII] 1661,1666 emission lines in the UV, we can obtain a very secure measurement of the C/O ratio in HII regions. Recent campaigns have been successfully using this method to measure C/O abundances in dwarf galaxies using HST/COS, however, extremely metal poor galaxies (XMPs; 12+log(O/H) < 7.3 or < 3% solar) are notoriously rare and have challengingly faint emission, and so no significant measurements of C/O yet exist for the most metal-poor nearby galaxies. The recent discovery of unexpectedly strong ultraviolet OIII] 1666 and rare NIII] 1750 emission from the HST/COS G160M spectrum of nearby XMP galaxy, Leo P (12+log(O/H)=7.17), reveals a unique opportunity to measure the CNO abundances in a chemically-young, high-ionization galaxy with exceptionally bright emission. We propose HST/COS G140L observations of Leo P to simultaneously measure the C, N, and O abundance in the most metal-poor XMP to date. These observations will allow us to (1) anchor the C/O and C/N relationships by extending the low-metallicity baseline, (2) explore the potential continuity in C/O versus O/H from dwarf galaxies to DLAs, (3) test the proposed link between C and N production, and (4) help constrain rest-frame UV emission-line diagnostics in chemically-young systems in preparation for the distant galaxies that will be observed with JWST. In order to anchor the poorly constrained low-metallicity regime of the C/O-O/H relationship, we will use HST/COS spectroscopic measurements of the OIII] 1661,1666 and CIII] 1907,1909 emission lines of the extremely metal-deficient Leo P galaxy. This data will provide a crucial constraint on the C/O relationship in metal-poor dwarf galaxies, which yields important information on the time evolution and nucleosynthetic origins of these elements, and will provide an important template for early galaxy evolution. The most efficient observing strategy for these observations is to use the G140L grating on COS with the 1280 central wavelength setting, which allows simultaneous observations of all the necessary UV emission lines within Segment A. We have excellent input coordinates centered on the NUV surface brightness peak of the O-star Leo P from previous HST/COS observations, allowing us to utilize the time-efficient ACQ/IMAGE mode for target acquisition. Note that while the resolution of COS spectra is degraded for non-point sources, we have demonstrated in Berg+19 that the OIII] doublet is easily resolved and the CIII] doublet can be deblended in G140L spectra (allowing for an estimate of the CIII] electron density), even for targets with extended nebular emission that fills the COS aperture. We split our awarded 16 orbits up into 4 visits based on the updated COS guidelines to reduce observation failures. Our team is composed of the world's leader in studies of the CNO abundances in dwarf galaxies, resulting is many publications over the years. In particular, over the past several years, PI Danielle Berg has used HST/COS to bring about a renessaince of C/O abundance studies in nearby dwarf galaxies (Berg+16, Berg+19a, Berg+19b), while Evan Skillman has been studying UV abundances in HII regions for several decades, helping to pioneer the field of HII region C/O abundances in the 1990s (e.g., Garnett+95, Garnett+99, Kobulnicky & Skillman 1997, Kobulnicky & Skillman 1998). Additionally, John Chisholm and Kristen McQuinn bring complementary expertise of the stellar populations in Leo P (McQuinn+13; HST-GO-15967, PI Chisholm). Finally, all five members of our team: Danielle Berg, John Chisholm, Kristy McQuinn, Grace Telford, and Evan Skillman, are seasoned experts at analyzing COS UV and optical spectroscopy of star-forming galaxies, and detailed abundance modeling. Given our team's expertise, as well as being leaders of the Leo P optical abundance studies (Skillman+13), SFHs and metal retention determinations (McQuinn+13,McQuinn+17), and the HST/COS G160M data (PI Chisholm), we are distinguishably qualified to carry out the proposed project and nebular analysis. Galaxies Stellar Populations and the Interstellar Medium 6 false false true false false false false SUPPORTED GALAXY DWARF COMPACT YES J2000 J2000 Galex NUV: 18.81 The scheduling data was generated by CASM 30.1. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G140L 1280 The scheduling data was generated by CASM 30.1. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G140L 1280 1657806371743 The scheduling data was generated by CASM 30.3. 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