0Assigned ID: 6839
----- Attempting Submission 1 (Thu Apr 10 23:27:14 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.
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.
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.
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.
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.
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.
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.
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.
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.
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.This addresses the concerns raised by Ravi Sankrit:
(i) We need an updated Phase II, using all four FPPOS for targets 1, 3, 4, 5, 6 (same visit numbers) and 13 (visit 19) - now done.
(ii) We need further information for targets 3 and 6 regarding the acquisition - updated ETCs for acquisition based on HST/COS FUV fluxes.-2050794764----- Attempting Submission 1 (Mon Aug 18 22:29:45 GMT 2025) -----
----- Attempting Submission 2 (Tue Dec 30 18:18:26 GMT 2025) -----There are two flavor of warnings:
(1) Warning (Form) COS FUV PSA science exposures with extended targets have special calibration limitations.
This should be fine.
(2) Warning (Form) 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).
I addressed this for the targets requested.A New Benchmark Set of Massive Stars Spectra to Distinguish Wolf-Rayet Stars and Very Massive StarsDetermining the stellar content of UV-bright star-forming galaxies is crucial to understanding the origin and evolution of massive stars and their impact on their host galaxies across cosmic time. Despite the importance of massive stars, current stellar population synthesis models cannot reproduce a number of stellar and nebular spectral features in high-ionization galaxies, e.g., broad HeII emission. We propose HST/COS far-UV spectra covering 913-1940 angstroms for 14 integrated star-forming regions and galaxies. These spectra will probe a suite of wind features that are sensitive to the very-massive-stars (VMSs) and classical Wolf-Rayet stars (cW). While the vast majority of far-ultraviolet (FUV) stellar studies to date focused on wavelengths >1300 angstroms, the extension of the proposed spectra to the very-blue FUV (< 1300 angstroms) is essential to capture the high-ionization features sensitive to the youngest ages, capable of distinguishing the presence of the most extreme young VMSs from the more evolved cWRs. These data will be used to construct the first FUV spectral catalog of integrated star-forming regions that can diagnose the presence of, and distinguish between, WRs and VMS. This atlas will provide crucial benchmarks for stellar population models to accurately constrain the relative importance of the most extreme and massive stars.Goal:
We will obtain NUV target aquisiton images and high S/N HST/COS G140L/800 FUV spectra of the suite of 914-1940 angstrom stellar continuum features that are sensitive to the contributionsfrom VMSs and WRs.
Targets:
Our targets were selected from previous galaxies and HII regions with optical spectra showing strong, broad (> 500 km/s) He II 4686, that are UV-bright, and which sample a range of metallicities and ionization parameters. The sample contain 7 cWRs targets, which demonstrates strong blue and/or red WR bumps and 7 VMSs targets, which lack a clear blue or red bump.
Acquisition:
Our sample benefits from having two of the following: (1) previous HST/COS observations, (2) UV HST imaging, and (3) PanStarrs imaging, providing very accurate coordinates. The three targets in our sample without HST observations have PanStarrs coordinates, which are generally accurate to 0.1". The excellent input coordinates of our sample allow us to utilize the ACQ/IMAGE mode for target acquisition with the PSA aperture and Mirror A/Mirror B (for half of the targets each) for the COS/NUV configuration.
Science Exposures:
HST/COS spectra will be taken with the G140L grating with the 800 central wavelength setting to cover ~913-1940 angstroms, which allows simultaneous observations of all necessary UV stellar features. This provides a resolution of R=1500-4000, or a velocity resolution of 75-400 km/s, which is sufficient to resolve the stellar continuum wind features of the proposed galaxies. We used the COS ETC to determine the time needed to achieve S/N>5-10 per resel element in G140M/800. These calculations were optimized to achieve S/N near OVI at 1032,1038.PI Danielle Berg is an expert on the spectroscopic properties of star-forming regions and galaxies. She has led many HST/COS UV spectroscopy programs of star-forming galaxies, including CLASSY, a Large HST program connecting the properties of the massive star populations with the gas properties of the host galaxies.
Co-I John Chisholm is an expert on the UV properties of star-forming galaxies in the local universe and at high redshift, with special expertise and publications on the properties of massive star populations from their UV spectra. He is the PI of the first program ever to observe extremely metal-poor massive star FUV spectra. He is also a co-PI of the CLASSY project, and a member of the MEGASAURA team.
Co-I Claus Leitherer is an expert on stellar population synthesis models and has a strong background in stellar atmosphere and evolution models. He led led the development and release of the original version of Starburst99 in 1999.
Co-I Andreas Sander is a world expert on massive stars and is a co-developer of the PoWR stellar atmosphere code for WR stars and has strong expertise in the interpretation of the spectra of hot stars.
Co-Is Paul Crowther is a world expert on massive stars, including very massive stars and wolf-rayet stars. He has led many of the foundational spectroscopy programs and has extensive experience interpreting FUV spectra.
Co-Is Evan Skillman, Karla Arellano-Cordova, Noah Rogers, and Richard Pogge are experts of star-forming galaxy evolution and nebular spectroscopy. They have extensive expertise in UV and optical spectroscopic studies of HII regions and star-forming galaxies. Skillman and Pogge are also the co-PIs of the CHAOS survey, which several of the targets were selected from. Pogge is an expert at all things related to radiative processes. His expertise will be critical to understanding the conditions which can produce the stellar featutes we observe.GalaxiesStellar Populations and the Interstellar Medium6falsetruefalsefalsefalsefalseSUPPORTEDISMHII REGIONYESJ2000J2000FUV = 15.0ISMHII REGIONYESJ2000J2000FUV = 14.7ISMHII REGIONYESJ2000J2000FUV = 16.3EXT-MEDIUMHII REGIONNOJ2000J2000FUV = 16.4, NUV = 17.2ISMHII REGIONYESJ2000J2000FUV = 14.5, g=15.98ISMHII REGIONYESJ2000J2000FUV = 16.6ISMHII REGIONYESJ2000J2000FUV = 16.2EXT-MEDIUMHII REGIONNOJ2000J2000FUV = 17.1ISMHII REGIONYESJ2000J2000FUV = 14.0, NUV = 16.51EXT-MEDIUMHII REGIONNOJ2000J2000FUV = 17.3ISMHII REGIONYESJ2000J2000FUV = 16.4EXT-MEDIUMHII REGIONNOJ2000J2000FUV = 16.7, NUV = 18.17EXT-MEDIUMHII REGIONNOJ2000J2000FUV = 15.6, NUV = 17.54EXT-MEDIUMHII REGIONNOJ2000J2000FUV = 17.9, NUV = 18.67COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG140L800COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG140L800COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG140L800COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG140L800COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG140L800COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG140L800COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG140L800COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG140L800COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG140L800The scheduling data was generated by CASM 33.1.CASM was run in Phase II mode./Users/dab5467/Downloads/OP-cache/PHASEII-v01.xml(Tic-Visit
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