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: 4850
----- Attempting Submission 1 (Wed May 24 23:52:26 GMT 2023) -----
Our observations will be conducted at LP6; warning thus ignored.
INEFFICIENT ORDERING OF FP-POS POSITIONS
Resubmission with approved 3-orbit repeat visit.
(still applies 2025-03-27:) We acknowledge the 'inefficient ordering of FP-POS positions' warning; but this is not relevant to our program configuration as the grating setting changes occur during occultation.
1775414262
----- Attempting Submission 1 (Thu Sep 14 00:42:24 GMT 2023) -----
----- Attempting Submission 2 (Thu Mar 27 20:06:43 GMT 2025) -----
The inefficient ordering warning is not relevant to our program as the grating setting changes occur during occultation and thus produce no integration time penalty.
Mega-deep UV spectroscopy of star-forming galaxies: completing the picture of the extremely metal-poor massive stars underlying high-ionization UV nebular emission
Local star-forming dwarf galaxies provide the only laboratory in which extremely metal-poor stellar populations like those encountered at the highest redshifts can be studied in detail. Over hundreds of orbits, Hubble has completely revolutionized our view of young star-forming systems, extending our ultraviolet vision to substantially younger ages and lower metallicities than previously seen. This exploration has revealed a rare population of extremely metal-poor systems dominated by massive stars that power UV nebular emission lines at strengths approaching that encountered in the first JWST spectra at z>~9. Unfortunately, the existing local UV spectra leave the faint continuum signatures of these massive stars effectively unconstrained in the lowest-metallicity and most extreme nebular emitters. Here we propose to remedy this by completing extraordinarily-deep 40-50 orbit spectra for the two brightest star forming regions known that are likely to harbor massive stars at or below 5% solar. These spectra will directly constrain the stellar photospheric and wind signatures imprinted on the FUV continuum which hold the key to understanding the hot stars that dominate high-ionization nebular line emission. Comparing these galaxies to stellar population synthesis prescriptions will provide our best hope of empirically calibrating the models that will continue to be used routinely at high-redshift in the coming years. Without these crucial UV observations, our understanding of the highest-redshift and lowest-mass systems that JWST and the ELTs will uncover will suffer from substantial systematic model uncertainties unaddressable without a UV space telescope.
This program will acquire deep FUV spectroscopy in a single grating setting for two galaxies, which represent the UV-brightest star-forming complexes at extremely low-metallicities <5% solar and young ages <~5 Myr. This data will be carefully combined with previous HST/COS investment to build the highest-SNR view possible of the FUV continuum of such young metal-poor massive star populations. We leverage these previous observations and their SDSS coverage in designing this program.
Coordinates and acquisition: Each target is a compact source whose core (the target of our observations) is unresolved in ground-based imaging. The target coordinates are derived directly from the ICRS-aligned SDSS photometry. To optimize the target acquisition exposures, we examine the existing ACQ/IMAGE exposures of each taken with COS previously. We sum the countrate within ~0.24'' of the centered target coordinates in each, which we find to be reasonably constant across different images and differ by approximately the same fraction as the target fluxes in the FUV as-expected. Then, we compute a time for the new standardized acquisitions by estimating the integration necessary to build-up 3000 counts in this central core, which delivers a conservative Poisson-only SNR of 55. We confirm that these exposure times (108 and 69s) would also yield anticipated SNR>>20 assuming a perfect point source flat in AB with a target flux set to the level measured in existing FUV spectra; and note that the galaxies have been successfully acquired with similar or shorter exposure times previously.
Observing plan: Our objective relies on maximizing data quality and total integration time, which will place us in the SNR>20 / resel regime (SNR~30 / resel after combination with existing data). We thus optimize for orbit-long dwells at fixed FP-POS position to minimize overheads. Full buffer dumps and auto wavecals are thus performed during occultation (with the exception of the first integration of a visit after the target acquisition). We block all observations into 3 orbit visits (plus two single-orbit visits to complete the allocation) for maximum schedulability while minimizing overheads. FP-POS settings are cycled between visits to achieve near-uniform integration at all four settings.
Safety: Both objects have previously been observed with the exact same COS target acquisiton & spectroscopic configuration without issue.
The assembled team has extensive experience using HST/COS to study nearby dwarf galaxies with medium-resolution FUV+NUV spectroscopy. Over the past six cycles, members of our team have successfully led many proposals targeting similar samples of star-forming dwarfs with COS spectroscopy and published the results expediently (GO:14168, 14679, 15646, 15881, PI: Stark; GO: 17198, PI: Senchyna; GO: 13312, 14628, 15422, 15465, PI: Berg; and the CLASSY Treasury Program GO: 15840, PI: Berg, Co-PI Stark). Results from these programs have been published in Senchyna et al. 2017, 2019, 2021, 2022, 2023; Berg et al. 2016, 2019a,b, 2021; Chevallard+2018; and several in-preparation manuscripts. The proposed COS G160M observations are very similar in nature to the G160M data collected in these previous programs, and will be reduced and analyzed using the techniques we have developed and tested already.
PI Senchyna and Co-I Stark 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. The team has already built the infrastructure necessary to robustly extract constraints on the stellar metallicity and age from such deep FUV spectra, which will be applied to the new data. PI Senchyna and Co-I Chisholm are experienced massive star continuum modelers, and will lead analysis of the continuum fits and comparison to both diverse models and other UV stellar samples. Co-Is Stark, Berg, and Sanders are experts in the measurement and interpretation of high-ionization nebular emission lines and , and will drive the interpretation of these population constraints alongside the nebular line measurements in the context of high-redshift and local galaxies as well as nebular gas and chemical evolution models. Co-Is Jones and Chisholm are experts in outflow modeling, and will lead the linkage of the massive star and nebular constraints to the outflowing gas detected in these and other existing COS spectra. Co-Is Chevallard, Charlot, and Plat have developed a full suite of both population synthesis + nebular photoionzation models and a robust model comparison framework, and will lead comparison of the nebular line strengths to those predicted by the population synthesis models constrained by the continuum. They will also lead direct fits to the entire data using their tool BEAGLE (Chevallard & Charlot 2016), simulating and stress-testing techniques applied to lower-S/N data at high redshift.
Galaxies
6
false
true
false
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SUPPORTED
GALAXY
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G160M
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COS/FUV
Spectroscopic
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No
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