For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. 0 Assigned ID: 7437 ----- Attempting Submission 1 (Thu Apr 16 16:07:21 GMT 2026) ----- HST Phase I Proposal 7437 successfully submitted. Receipt: # 7437-1 ----- Attempting Submission 2 (Thu Apr 16 20:20:29 GMT 2026) ----- HST Phase I Proposal 7437 successfully submitted. Receipt: # 7437-2 ----- Attempting Submission 3 (Thu Apr 16 22:58:23 GMT 2026) ----- Can use default LP6 with G160M. For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser. 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. For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser. 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. 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. 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. 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. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. 0 ----- Attempting Submission 1 (Mon Aug 17 15:55:28 GMT 2026) ----- The targets are extended galaxies observed through the COS PSA. We acknowledge the associated limitations in FUV flux calibration and spectral resolution. For the G160M observations split between Visits 01 and 02, all four FP-POS positions are used collectively across the two visits. The First UV-Based Metallicity Constraints for AGN Dwarf Galaxies Nearby dwarf galaxies hosting AGN provide a rare local laboratory for studying black hole formation and growth in the low-mass regime. Yet the metallicities of their narrow-line regions (NLRs) remain unconstrained. This is a major gap because NLR metallicity traces the chemical state of the gas surrounding the accreting black hole and encodes the effects of black hole growth, star formation, inflows, and outflows. In AGN, however, metallicity cannot be measured directly and instead must be inferred from a combination of emission line ratios and photoionization models. Optical spectra alone do not adequately constrain the gas density, abundance patterns, and ionization structure required to make those models reliable, especially for the conditions expected in dwarf AGN. We propose 32 orbits of HST/COS G160M+G185M spectroscopy of five dwarf AGN to obtain the UV diagnostics needed to break these degeneracies and place the first robust UV-based metallicity constraints on a sample of dwarf AGN. These observations will provide the density, abundance, and ionization constraints needed for reliable NLR metallicity measurements, filling a key gap in our ability to interpret the effect of AGN in low-mass galaxies. This program will establish the physical framework needed to understand the growing dwarf AGN population and assess how black holes shape the chemical evolution of low-mass galaxies. We observe five nearby dwarf AGN with COS/G160M and G185M through the Primary Science Aperture. The target-specific central wavelengths were selected to provide coverage of the redshifted C IV, He II, O III], and C III] emission lines while avoiding detector gaps. Each visit begins with a COS/NUV ACQ/IMAGE exposure to center the UV nucleus. MIRRORA is used for the fainter acquisition targets, while MIRRORB is used for the two brighter targets All science exposures are obtained in TIME-TAG mode. The G160M observations use both FUV detector segments at LP10 and are divided among all four FP-POS positions to reduce fixed-pattern noise. Multiple FP-POS positions are also used for G185M. The observations are divided into 11 visits of three orbits or fewer, for a total of 32 orbits. The acquisition and science exposure times are based on COS ETC calculations, and buffer times are chosen following the COS TIME-TAG recommendations. According to the Bright Object Tool (BOT), there are no bright sources near our targets that could cause a problem for COS. Proposal PI Aravindan in experienced observational studies of AGN in dwarf galaxies, and has led papers discussing the efficacy of AGN-driven outflows in dwarf galaxies (Aravindan et al. 2023, 2026). She also works on quantifying the effects of AGN feedback in dwarf galaxies using high ionization emission lines and identifying improved methods to detect AGN in low-mass galaxies (Aravindan et al. 2024). She has also been a Co-I of several approved HST programs on characterizing AGN feedback in dwarf galaxies. Co-I Berg is a leading expert in nebular gas diagnostics and the chemical enrichment of star-forming galaxies, especially of CNO abundances (Berg et al. 2016, 2018, 2019a, 2019b, 2021, 2022, 2024, 2026). Co-I Berg has also pioneered observational campaigns of rest-UV+optical emission, in both the local universe and at high-redshifts. In particular, co-I Berg has been leading the field in detecting and characterizing extreme emission line galaxies and co-PIed the CLASSY Treasury Survey. Co-I Chisholm is an expert on characterizing massive, metal-poor stars and stellar populations in Local Group dwarf galaxies, and co-leads the JWST-GLIMPSE program, dedicated to probing the faintest and earliest galaxies in the Universe and their properties. He is an expert in HST/COS ultraviolet spectroscopy and in using UV diagnostics to constrain the ionization structure and outflow properties of nearby dwarf galaxies (Chisholm et al. 2016a, 2016b, 2021) Co-I Martinez has significant experience deriving physical gas conditions, determining total and relative abundances, and photoionization modeling to interpret the properties of extreme N-emitters across cosmic time (Martinez et al. 2025). Co-I Canalizo is an expert in AGN, their host galaxies, and their environments, including the connection between mergers, starbursts, and AGN activity, and the coevolution of BHs and their host galaxies. Supermassive Black Holes and Active Galaxies Galaxies 6 false false false false false false false SUPPORTED GALAXY NUCLEUS SEYFERT YES This object was generated by the targetselector and retrieved from the SIMBAD database. 2MASX-J08514952+4247180 J2000 J2000 GALEX NUV=18.299 FUV=18.875 GALAXY NUCLEUS SEYFERT YES This object was generated by the targetselector and retrieved from the SIMBAD database. 2DFGRS-TGN420Z105 J2000 J2000 GALEX NUV = 18.219 FUV = 18.799 GALAXY NUCLEUS SEYFERT YES This object was generated by the targetselector and retrieved from the SIMBAD database. Z-291-32 J2000 J2000 GALEX NUV=16.733 FUV = 16.958 GALAXY NUCLEUS SEYFERT YES This object was generated by the targetselector and retrieved from the 2MASS database. 12204209+2920452 J2000 J2000 GALEX NUV=16.927 FUV =17.627 GALAXY NUCLEUS SEYFERT YES This object was generated by the targetselector and retrieved from the SIMBAD database. LEDA-1702471 J2000 J2000 GALEX NUV=18.281 FUV=18.584 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Spectroscopic No No G185M 1850 COS/FUV Spectroscopic No No G160M 1589 COS/NUV Spectroscopic No No G185M 1864 COS/FUV Spectroscopic No No G160M 1600 COS/NUV Spectroscopic No No G185M 1835 COS/FUV Spectroscopic No No G160M 1600 COS/NUV Spectroscopic No No G185M 1817 COS/FUV Spectroscopic No No G160M 1589 COS/NUV Spectroscopic No No G185M 1882 /private/var/folders/gj/2w4j5xcd5x15xxvn9z1rsv2m0000gq/T/OPVisit15598509420684507269.xml The scheduling data was generated by CASM 34.2. CASM was run in Phase II mode. 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