0Assigned ID: 6299
----- Attempting Submission 1 (Wed Apr 09 22:07:08 GMT 2025) -----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.We have completed to the best of our ability the Phase II for this program. We note that the BOT for 12 of the 15 targets (based on the GALEX catalog) are fine, but three of the sources do not have GALEX coverage and have warnings when based on GS II. We have specified realistic SEDs for these sources in our ETCs, which we cite in the Phase II. These SEDs are based on detailed SED fitting of archival data spanning the u-band to mid-IR and more details are available upon request.
Resubmission note: Due to a duplication of one of our previous targets, we have now added J132549.42+330354.3 to this submission (to replace J135950.93+572623.0).
Nov 1, 2025: Updated buffer times for all COS exposures.
Apr 2, 2025: I've duplicated the failed observation from visit 12, now visit 16.1459708786----- Attempting Submission 1 (Tue Aug 12 20:42:37 GMT 2025) -----
HST Phase II Proposal 18099 successfully submitted.
Receipt: # 18099-1
----- Attempting Submission 2 (Fri Aug 22 18:31:09 GMT 2025) -----
HST Phase II Proposal 18099 successfully submitted.
Receipt: # 18099-2
----- Attempting Submission 3 (Sat Nov 01 15:52:13 GMT 2025) -----
HST Phase II Proposal 18099 successfully submitted.
Receipt: # 18099-3
----- Attempting Submission 4 (Thu Apr 02 18:22:15 GMT 2026) -----The warnings in this APT have to do with the targets being extended. All of our calculations have accounted for this, as outlined in the proposal and APT comments.Uncovering the Ionizing Sources in Metal Poor Galaxies: UV Spectroscopy of an X-ray Observed SampleRecent investigations have shown that star-forming galaxies (SFGs) show signatures of hard ionizing spectra (based primarily on the presence of nebular He II 4686), with a rising fraction of SFGs showing these signatures with decreasing metallicity. While stellar population models struggle to reproduce these emission lines, emerging binary population synthesis models are showing promise in reproducing these spectral signatures. In this proposal, we aim to obtain critical UV spectroscopy with HST/COS (G140L) for a legacy sample of 15 metal-poor SFGs (MPGs) with Z ~ 0.03-0.2 Zsol that have or will have securely measured X-ray properties and span a range of optical ionization conditions. UV spectroscopy will provide unique emission/absorption-line diagnostics that aid in characterizing the stellar and nebular conditions, including photoionization versus shock signatures, ionizing spectral hardness, and stellar population ages that cannot be obtained from optical spectra. We will simultaneously model the UV spectra along with rich multiwavelength data suites from X-rays, SDSS spectra, and UV-to-IR photometry to obtain complete pictures of the shapes of intrinsic ionizing continuua of these galaxies, their detailed star-formation histories, and the role that binary populations play in powering extreme emission lines.We will conduct COS observations of an X-ray observed sample of 15 metal-poor star-forming galaxies (MPGs). We will use the COS FUV G140L/1105 Angstrom grating for our observations. This choice allows for the detection of features related to hard ionizing spectra (when present), including C iv 1550, He ii 1640, O iii] 1666, (when strong) C iii] 1908, as well as Lyalpha for our full sample (redshifts z = 0.017-0.045). NUV acquisition images of the targets will be obtained with Mirror B and the ACQ/IMAGE mode to reach a S/N > 15 inside a 9x9 pixel box centered on the brightest part of the galaxy. The MPGs satisfy safety conditions for observing with the COS, including lacking bright sources within a 43 arcsec diameter surrounding the sources. We estimated UV spectra exposures using the ETC, requiring S/N > 5 in the continuum at 1550 Angstrom. While our MPGs are compact in size, <= 40% of their total FUV fluxes will lie outside of the COS aperture. For the ETC we conservatively used 50% of the objects' total FUV fluxes, showing that exposures of ~500-3,000 s (1-2 orbits) are sufficient for our program.Data reduction, analysis, and interpretation will be done as in our previous GO 13744, GO 14635, GO 15136, GO 15639, GO 15941, GO 16271, and GO17100 projects and documented in Izotov et al. (2016a,b, 2018b,c, 2020, 2021b, 2023, 2024). Our team includes experts on all relevant aspects and disposes of all necessary tools, including a custom pipeline for faint COS spectra (Makan et al. 2021), SED fitting tools and development (Monson et al. 2022, 2023; Lehmer et al. 2024), X-ray data analysis and interpretation (e.g., Lehmer et al. 2019, 2020, 2021, 2022, 2024), modeling of nebular emission with Cloudy (Amiri et al. 2022, 2023) and more. Our team led the recently accepted large Chandra proposal that is ongoing and observing many of the targets here. All galaxies possess SDSS spectra with which Izotov derived data such as nebular line ratios, Hbeta and HeII emission-line luminosities, starburst ages and masses, limits on photoionization by WR stars and shocks, element abundances, specific star formation rates, etc. All galaxies will contain X-ray data sets that will be studied in conjunction with SED fitting techniques. 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