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Assigned ID: 982
----- Attempting Submission 1 (Fri Apr 05 23:45:59 GMT 2019) -----
HST Phase I Proposal 982 (Low_Metallicity_Stars_HST_submited.pdf.apt) successfully submitted.
Receipt: # 982-1
Updated the coordinates for the Sextans A star.
613719094
----- Attempting Submission 1 (Tue Jul 23 13:26:26 GMT 2019) -----
HST Phase II Proposal 15967 (Low_Metallicity_Stars_HST_submited.pdf.apt) successfully submitted.
Receipt: # 15967-1
----- Attempting Submission 2 (Thu Jul 25 17:15:00 GMT 2019) -----
HST Phase II Proposal 15967 (Low_Metallicity_Stars_HST_submited.pdf.apt) successfully submitted.
Receipt: # 15967-2
----- Attempting Submission 3 (Mon Nov 04 12:04:46 GMT 2019) -----
HST Phase II Proposal 15967 (Low_Metallicity_Stars_HST_submited.pdf.apt) successfully submitted.
Receipt: # 15967-3
----- Attempting Submission 4 (Mon Nov 11 17:00:49 GMT 2019) -----
Constraining the Stellar Astrophysics Powering Cosmic Reionization: Spectral Templates of Extremely Low-metallicity Main-sequence O-stars
Massive stars are thought to have contributed to the reionization of the early universe, however very little is known about the stellar astrophysics of the extremely low-metallicity massive stars that produced the requisite ionizing photons. Crucially, the photospheric opacities and stellar wind mass-loss rates have not been observationally determined below SMC metallicities (0.2 solar). This leaves estimates of the intrinsic number of ionizing photons produced by low-metallicity massive stars largely unconstrained. Consequently, high-redshift observations with JWST will be unable to distinguish between models that power reionization with stars or active galactic nuclei, unless the stellar physics is determined. Here, we propose 49 orbits of HST/COS far-ultraviolet moderate resolution spectroscopy with G130M and G160M of the three known extremely low-metallicity (3-10% solar) main-sequence stars in dwarf galaxies around the Milky Way. The close proximity of these galaxies enables observations of single O-stars to determine the stellar wind mass-loss rates and the photospheric compositions, mainly the iron abundance which is the chief O-star opacity source. As the only known isolated main-sequence O-stars at these metallicities, these observations will be suitable for inclusion in stellar libraries and test stellar astrophysical theory at extremely low-metallicities. These 49 orbits will complement the planned ULLYSES by extending the observations to lower metallicities than currently planned. In total, these observations will provide the first, and possibly only, direct constraints on the stellar astrophysics thought to be responsible for the reionization of the universe.
Here we plan observations of three very low-metallicity, main-sequence O-stars in the local universe with the Cosmic Origins Spectrograph. We will utilize both the G130M and G160M configuration to get continuous coverage of important stellar wind and photospheric features to determine the mass-loss rates and abundances of the lowest metallicity known single O-stars to constrain their output of ionizing photons.
We have checked target coordinates using GAIA DR2. GAIA has an astrometric error less than 0.1". There were slight pointing offsets and we have tightened our coordinate constraints to account for this.
We estimate exposure times using the V-band magnitude, observed interstellar reddening, point sources, and model fits for the SED shape. We have tested various O3 through O7 stellar templates in the COS ETC and confirm that the templates conservatively estimate the required exposure times. We use these estimates for the acquisition and exposure times. These extrapolations are conservative estimates on the total FUV flux. When available, we have compared to the observed FUV fluxes to confirm that these are conservative estimate.
We will use Mirror A for the acquisition. All of the acquisitions satisfy the GALEX safety standards. We organize the observations into visits of at most 5 orbits, to aid schedulability.
We use the G130M grating with the 1291 central wavelength. This covers the N V 1240, O V 1371, and Si IV 1400 stellar wind profiles. The G130M configuration only uses FP = 3, 4 configurations to satisfy the COS2025 restrictions. We then use the G160M grating with the 1600 central wavelength. This configuration covers the Fe V 1428, S V 1500, C IV 1550, He II 1640, Fe IV 1717, N IV 1719, and N III 1750 stellar wind and photospheric profiles. We use FP = All for the G160M observations to extend the possible wavelength coverage.
Our team is positioned to deliver timely and high-quality analysis of the planned observations. Combined the team has published 10 first-author papers that utilized data from the Cosmic Origins Spectrograph, including ten previously accepted HST-GO COS proposals. This ensures that we have intimate knowledge of COS data reduction and analysis.
CO-I Dr. Mcquinn has intimate knowledge of the three proposed dwarf galaxies, including extensively mapping the CMDs of the objects (Mcquinn et al. 2013, 2015).
Dr. Chisholm has extensive experience working with spatially unresolved observations of massive stars at both high and low metallicity (Chisholm et al. 2015, 2016, 2018, 2019) and will use this knowledge to measure the mass-loss rates and stellar photospheric absorption properties.
Combined our team will efficiently analyze and determine the stellar astrophysical properties of the possible sources of cosmic reionization.
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