0 Assigned ID: 1000 ----- Attempting Submission 1 (Fri Apr 05 23:52:43 GMT 2019) ----- HST Phase I Proposal 1000 (civcos.pdf.apt) successfully submitted. Receipt: # 1000-1 ----- Attempting Submission 2 (Fri Apr 05 23:57:11 GMT 2019) ----- HST Phase I Proposal 1000 (civcos.pdf.apt) successfully submitted. Receipt: # 1000-2 ----- Attempting Submission 3 (Fri Apr 05 23:59:32 GMT 2019) ----- ----- Attempting Submission 4 (Sun Apr 07 03:57:47 GMT 2019) ----- 0 ----- Attempting Submission 1 (Fri Jul 26 00:26:16 GMT 2019) ----- Ultra-Deep HST/COS Spectroscopy of Extremely Metal-Poor Galaxies The first glimpse of the spectra of z~7-10 galaxies has revealed intense nebular emission that has proven challenging to interpret owing to shortcomings in our understanding of low metallicity stellar populations. Recent work with HST/COS in the local universe has provided a way forward, characterizing the UV spectra that are common in metal poor galaxies. Attention to date has focused on the strongest CIV emitting galaxies found locally, as these appear most similar to the few detections known at z>6. But it has recently become clear that the majority of metal poor galaxies exhibit much weaker CIV. Nothing is known about the nature of the massive stars in these systems, resulting in an extremely biased view of the range of radiation fields powered by low metallicity stars in metal poor galaxies. Here we propose to combat this problem by providing the first study of the massive stars in the dominant population of metal poor galaxies in the local universe. Via deep (5 orbit) COS/G160M spectra of two of the z<0.02 metal poor galaxies with weak CIV emission, we will deliver quantitative constraints on the metallicity of massive stars through measurement of photospheric absorption lines and test stellar wind prescriptions in the poorly calibrated low metallicity regime. Using new spectral tools, we will test whether existing population synthesis models can simultaneously reproduce the metallicity and radiation field, providing a powerful stress test for models. If this UV database is not completed soon, the interpretation of reionization era galaxy spectra will be jeopardized throughout the JWST era. Our program will obtain ultra-deep medium-resolution FUV COS spectroscopy for two highly star-forming extremely metal-poor galaxies identified as producing anomalously weak nebular C IV emission. The target galaxies are compact, have high-precision coordinates confirmed in SDSS, and have been previously observed with lower-resolution COS spectroscopy. In order to make the program as flexible as possible in scheduling, we have broken the 5 orbits devoted to each galaxy into 3 separate visits. As in previous COS programs targeting similar galaxies, we will perform ACQ/IMAGE exposures to center the galaxies in the COS aperture. Then, each orbit will be devoted to integration at a single FP-POS setting, with buffer readout and grating shift occuring during occultation. Since readout occurs during occultation, we set the BUFFER-TIME to the exposure time to ensure the entire buffer is read. All observations will be conducted with G160M/1533, which gives simultaneous coverage of key stellar wind lines and photospheric features in the range 1350-1700 Angstroms yielding constraints on stellar wind strengths and stellar Fe abundance. In five orbits per object, we will achieve S/N per resolution element >4, providing confident measurement of these features and a comprehensive picture of the massive stellar populations in the target systems. The assembled team has extensive experience using HST/COS to study nearby dwarf galaxies with medium-resolution FUV+NUV spectroscopy. Over the past three cycles, we have suc- cessfully led four proposals targeting samples of star-forming dwarfs with G160M+G185M (GO:14168 in Cycle 23, 14679 in Cycle 24, 15185 in Cycle 25, and 15646 in Cycle 26; PI:Stark) and published the results of these programs expediently. Analysis of the first of these (14168) was presented in Senchyna et al. 2017 and Chevallard et al. 2018. Analysis of the second (14679) was presented in Senchyna et al. 2019. The observations and data analysis for GO: 15185 was recently completed and will be presented in a paper this coming Fall. The proposed COS G160M observations are very similar in nature to (but much deeper than) the G160M data collected in these previous programs, and will be reduced and analyzed using the techniques we have developed and tested already. PI Stark, Co-I Senchyna, and Co-I Jones are experienced with planning and analyzing HST/COS FUV spectroscopy of nearby dwarf galaxies, and will be responsible for data reduction and analysis. This will involve designing target acquisition and observing strategy, optimally combining exposures, and cleaning spectra of MW absorption lines. Co-Is Chevallard and Charlot have developed a full suite of both population synthesis models and a robust model comparison framework, and will lead comparison of these data to models using BEAGLE (Chevallard & Charlot 2016). This will involve both full-spectrum and isolated model comparison experiments, and will require an awareness of model limitations and HST/COS data subtleties that our group has developed. 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