0 Assigned ID: 5213 ----- Attempting Submission 1 (Mon Mar 25 18:19:17 GMT 2024) ----- HST Phase I Proposal 5213 successfully submitted. Receipt: # 5213-1 ----- Attempting Submission 2 (Tue Mar 26 10:44:28 GMT 2024) ----- HST Phase I Proposal 5213 successfully submitted. Receipt: # 5213-2 ----- Attempting Submission 3 (Tue Mar 26 10:46:37 GMT 2024) ----- HST Phase I Proposal 5213 successfully submitted. Receipt: # 5213-3 ----- Attempting Submission 4 (Tue Mar 26 18:35:02 GMT 2024) ----- HST Phase I Proposal 5213 successfully submitted. Receipt: # 5213-4 INEFFICIENT ORDERING OF FP-POS POSITIONS COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS We would be very grateful for your answers to our questions about FP-POS and Buffer time, see proposal description 1360648834 ----- Attempting Submission 1 (Thu Aug 15 21:12:39 GMT 2024) ----- 1. The targets have Gaia DR3 coordinates. Should we provide different coordinates? 2. Can you please advice how to improve teffciency of FP-POS. The sequence which is in the APT was produced by the apt. . UV spectroscopy of the complete sample of Wolf-Rayet stars in the low-metallcity galaxy NGC 6822 We propose the first UV spectroscopic study of the complete sample of four Wolf-Rayet (WR) stars in the low-metallicity galaxy NGC6822. WR stars are rare objects which represent the final evolutionary stage of most massive stars short before their collapse into black holes, and are important feedback sources. Low-metallicity WR stars are emigmatic but, arguably, the most important testbeds of the final stages of massive star evolution in conditions resembling those in the early Universe. The new COS spectra of the strategically important sample of low-metallcity WR stars are urgently needed to complement existing optical spectra, which by themselves are not sufficient to fully characterize these objects with strong winds. The HST data will be exploited to measure stellar and wind parameters using modern stellar atmosphere models. The determined mass-loss rates and wind velocities will be compared to those of WR stars in different galaxies, such as the Milky Way, the LMC, and the SMC, and used to anchor the metallicity dependence of WR wind strengths. The derived stellar parameters will test massive-star evolution models and allow a comparative study of low-metallicity WR stars in the SMC and NGC6822. If we find that WR stars in NGC6822 resemble the so far unique population of WR stars in the SMC (which fundamentally differs from the WR stars in galaxies with higher metallicity), it will disrupt the standard picture of black hole progenitors and stellar feedback at low metallicities, and by proxy in the young Universe. Obtaining the UV spectra of WR stars in NGC6822 is a necessary addtion to the HST legacy and will resonate across many areas of astrophysics. COS G140L spectra of four Wolf-Rayet stars in the galaxy NGC 6822. Four visits - one per target, 5 orbits each. The targets have V~ 20. The coordinates are from Gaia DR3. 1) The targets are relatively isolated, as also confirmed by the `target confirmation' tool. The ETC suggest small exp. times for img aqc, therefore we use this option. We hope this is fine. 2) We could not find optimum FP-POS, the apt gives warning on inefficient use. We would be very grateful for recommendation how to improve our strategy 3) We indicate buffer time 10000 sec, ie. 2/3 of buffer time calculated by the ETC. But we are not sure this is the optimum option and would be very grateful for your recommendations. The team consists of experts in all aspects described in the proposal. Drs. W-R Hamann and Sander are principal developers of non-LTE stellar atmosphere code PoWR which is one of the most common tool worldwide for the analyzies of Wolf-Rayet star spectra. Dr. Todt is expert in WR-stars and models stellar atmopsheres. Dr. Oskinova is expert in the UV observations and extragalactic massive star observations. Dr. Shenar and Dr. Ramachandran are the experts in metal poor massive stars and stellar feedback. Dr. Massa is an expert in COS observations of massive star winds. Mr. Pauli and Mr. Lefever are PhD students working on stellar winds and evolution of WR stars in low-metallicity galaxies. Stellar Physics and Stellar Types 6 false false true false false false false false SUPPORTED STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 COS/FUV Spectroscopic No No G140L 800 /tmp/OPVisit2818869131963303981.xml The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. 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