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.0Assigned ID: 5869
----- Attempting Submission 1 (Tue Mar 26 23:54:21 GMT 2024) -----Confirming our program can proceed with LP6.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.
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.
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.
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.
INEFFICIENT ORDERING OF FP-POS POSITIONS
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.
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.
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.
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.
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.
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.
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.Repeats for exposures of J013911.93+154241.3 that suffered guide star acquisition loss per HOPR 93407. Warnings regarding FP-POS settings are acknowledged, but we are allocating as equal time as possible across all four FP-POS positions and grating changes don't add overhead as they occur outside of target visibility.-266410266----- Attempting Submission 1 (Thu Aug 15 00:24:36 GMT 2024) -----
----- Attempting Submission 2 (Thu Dec 11 23:27:53 GMT 2025) -----FP-POS changes occur during target occultation, so no observing time is lost due to inefficient orderingCompleting the picture of high-ionization UV emission powered by the most metal-poor massive star populationsWith JWST spectroscopic samples expanding at z>6, a mysterious class of object is becoming ever more commonplace. Several extremely prominent CIV emitters (>20A equivalent width) glimpsed prior with ground-based facilities have been confirmed; and alongside this emission, JWST has revealed peculiar emission in NIV] suggestive of nitrogen enhancements. Even more surprisingly, similar signatures have now been established in other galaxies including the two most luminous systems spectroscopically confirmed at z>10. This emission has invoked significant debate and its origins remain unclear; but HST is poised to shed light on this mystery. After over a half-decade long search, HST/COS has finally identified two nearby galaxies that power CIV >20A, at the lowest metallicities (<5% solar) and youngest ages (<~2 Myr effective ages). These galaxies represent our best hope of understanding the processes underlying this emission at z>6, but only limited conclusions can be drawn from a sample of two. Here we propose to target the brightest remaining sources known at these youngest ages and lowest metallicities, and increase the sample of these best reionization-era analogues to five. By extending observations to targets at similar ages and metallicities but with a range of gas conditions, we will place the firmest possible statistical constraints on the ionizing spectrum and enrichment powered by the youngest extremely metal-poor stellar populations. These observations will complete the baseline critical for interpreting the spectra of the highest-redshift galaxies, and cement this sample as legacy benchmarks for the next generation of stellar population synthesis model development.This program will acquire FUV spectroscopy designed to constrain high-ionization nebular emission including in C IV and He II for three extremely metal-deficient nearby dwarf galaxies dominated by very young stellar populations. The targets are each covered by SDSS and GALEX imaging which we leverage in planning their observation.
Coordinates and acquisition: Each target is a compact source unresolved in ground-based imaging. The target coordinates are determined from the SDSS photometric outputs and confirmed to agree with the peak of u-band emission for each target in the ICRS-aligned SDSS imaging. Each target is thus acquired with a standard ACQ/IMAGE exposure, with exposure time chosen to deliver S/N=25 for a point source with an NUV AB magnitude equal to the faintest of the u-band fiber and cModel magnitudes (assuming a flat continuum in F_nu, appropriate for such sources). We confirm that all three have GALEX/NUV magnitudes brighter than this conservative estimate; and to ensure detector safely, we likewise confirm that no warnings are raised for a Mirror A+PSA observation of a point source with the brightest GALEX/NUV magnitude among the three. Based upon previous observations of similar sources, we expect these targets to be more extended than a point source, but with FWHM at NUV wavelengths significantly smaller than 0.6''; and we expect the requested SNR=25 exposures will deliver images adequate for precise acquisition without expending too large a fraction of the first orbit of each visit on alignment.
Observing plan: Our primary objective is nebular line measurement; our observations are thus in the low-S/N regime (<5 /resel in the continuum). To maximize the exposure time on-source, we thus devote each orbit to a single spectroscopic exposure, which enables us to relegate most of the buffer dump and expensive SPLIT wavecal overheads to occultation. All FP-POS positions are observed at least once for each object, and we endeavor to spread exposures as equally between the FP-POS settings as possible witin this scheme. A full buffer dump is requested for each exposure given the uncertain FUV countrates and the lack of impact on overheads. The warnings about inefficient FP-POS orderings are ignored as the grating shifts in all cases occur during occultation and thus have no impact on science exposure time.
Safety: The targets are all faint and have no UV-bright (<20 AB) nearby (<1 arcmin) neighbors, as confirmed with GALEX imaging catalogs. No health and safety warnings are issued by the BOT or other tools. Testing the ETC with conservative over-estimates of brightness (several magnitudes brighter than the brightest measured GALEX NUV magnitude) suggest no issues with exceeding countrate limits or filling the buffer too early with any of the target acquisition exposures or the spectroscopic integrations.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, 16677 PI: Stark; GO: 13312, 14628, 15422, 15465, PI: Berg; the CLASSY Treasury Program GO: 15840, PI: Berg, Co-PI Stark; GO:17198, 17475, 17526, PI: Senchyna). Results from these programs have been published in Senchyna et al. 2017, 2019, 2021, 2022, 2023; Berg et al. 2016, 2019a,b, 2021, 2022; 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. PI Senchyna and Co-Is Stark, Berg, Chisholm, and Chen are experts in the measurement and interpretation of high-ionization nebular emission lines, and will drive the measurement and interpretation of the CIV He II, NIV], and other lines targeted in the context of high-redshift and local galaxies as well as nebular gas and chemical evolution models. 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 measured in our data to state-of-the-art population synthesis 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.GalaxiesStellar Populations and the Interstellar Medium6falsetruefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONNOJ2000J2000GALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONNOJ2000J2000GALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONNOJ2000J2000COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1623The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.1759382489000206.74068595860035(Tic-Visit
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