0 Assigned ID: 3203 ----- Attempting Submission 1 (Fri Mar 25 12:19:50 GMT 2022) ----- HST Phase I Proposal 3203 successfully submitted. Receipt: # 3203-1 ----- Attempting Submission 2 (Fri Mar 25 18:06:28 GMT 2022) ----- HST Phase I Proposal 3203 successfully submitted. Receipt: # 3203-2 ----- Attempting Submission 3 (Fri Mar 25 18:11:26 GMT 2022) ----- HST Phase I Proposal 3203 successfully submitted. Receipt: # 3203-3 0 Assigned ID: 9106 ----- Attempting Submission 1 (Fri Mar 25 09:30:33 GMT 2022) ----- HST Phase I Proposal 9106 successfully transmitted Receipt: # 9106-1 For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. 0 ----- Attempting Submission 1 (Thu Jul 14 17:21:44 GMT 2022) ----- The proposal contains warnings regarding the mandatory use of all FFPOS. Some orbits use only 2 FPPOS, but we arranged the observations to make a balanced use of all 4 FPPOS. The winds of massive stars at the peak of the star formation history of the Universe Massive stars are powerful sources of ionizing radiation and kinetic energy that shape the interstellar medium and the UV spectral morphology of host galaxies. Their life-averaged feedback and their end as SN/GRB make them fundamental ingredients to galactic chemodynamical evolution models and population synthesis codes. Feedback from massive stars is not constant along the history of the Universe: their evolution and pre-SN core size is determined to a large extent by radiation-driven winds, and these depend strongly on metallicity. In a Universe of ever-increasing metal content, metal-poor massive stars and their winds are a central piece to study star-forming galaxies in past cosmic epochs. The HST archive, supported by the ULLYSES DDT program, stores a large collection of UV spectra of massive stars in the Milky Way and the Magellanic Clouds that will enable a thorough characterization of radiation-driven winds down to metallicities of 1/5 Zsun. Yet, this value is not representative of the composition of the Universe earlier than redshift=1, nor at such an important landmark as the peak of the Cosmic star formation history (redshift~2). We request HST-COS UV spectroscopy of 4 OB-type stars in Sextans A, with 1/10 Zsun metallicity, akin to blue massive stars of that period. The selection has been crafted to cover uncharted parameter space in the upper HR-diagram, where radiation-driven winds are expected to be significant. Quantitative analysis of this sample together with archival data will allow us to characterize radiation-driven winds at very low metallicity and to produce the first prescriptions to be implemented into models of stellar evolution. General strategy & summary -------------------------- This proposal consists of COS/FUV spectroscopy of 4 O-stars in the dwarf irregular galaxy Sextans A (at ~1Mpc). All targets are visited 3 times in order to accumulate exposure time. Visits have 3 orbits or less to facilitate scheduling. Science exposures: The configuration is COS/FUV, PSA, G140L, TIMETAG, FLASH=YES, CENWAVE=800 and SEGMENT-A (B is off by default). All FP-POS are used, although spread in several orbits/visits. Acquisition strategy: ACQ/IMH We checked that the sources are isolated in a radius of 2'' or that they are brighter than any other target in the r=2'' circle by more than 1 mag in the UV. To this aim we used WFPC3-F225W (preferred) or WFPC3-F275W phot. from program GO-16104 and imaging from Bianchi+ 2012. Source ID, Phot. and astrometric catalogs: ------------------------------------------- Alternate-ID-1 from Massey+ 2007, AJ, 133, 2393 Alternate-ID-2 from Lorenzo, Garcia, Najarro et al. accepted at MNRAS Source for optical photometry: Massey+ 2007, AJ, 133, 2393 Coordinates for the target stars were taken from Gaia eDR3. Estimated exposure times, Buffer times, and UV fluxes (Flux at 1300 Angstroems) ---------------------------------------------------------------------------------- The listed COS-ETC ID's for spectroscopy correspond to the ETC run with the following parameters. - COS ETC v30.2 - G140L, CENWAVE 800, segment-B HV-low, PSA - EXPTIME=2600s (roughly one full orbit) - Castelli & Kurucz models with the appropriate spectral type - LMC 30Dor supershell extinction law applied before normalization - Normalization by WFC3/UVIS VEGAMAG (F225W or F275W) from program GO-16104 (although exposure times and F_1300 were also calculated with observed V-magnitudes as a double check) These calculations provided - the input spectrum, were the estimated fluxes at 1300\AA were taken from - the buffer fill time (BFT), that was used to estimate the BUFFERTIME=2/3*BFT Extinction E(B-V) was estimated from observed optical UBV photometry, with intrinsic color (B-V)o calculated from the reddening-free Q-pseudo color following the relation by Massey+ 2000. For acquisition ETC quotes, the following parameters were used: - ACQ/IMAGE - PSA, MIRROR-A - GOAL: S/N=20 - With same parameters as above for input stellar spectrum and extinction law. Special requirements: --------------------- None requested. BOT checks: ----------- None of the ETC runs to estimate the exposure times for the spectroscopic science observations or the ACQ/IMAGE, returned any bright-object or count-rate warning. We ran APT's BOT tool, both with GSC2 and GALEX. BOT finds no unsafe objects in either of them. Only GSC2 showed Unknown sources. We queried UV photometry from program GO-16104 around their location and checked that all of them were fainter in the UV than F225W=17.34, F275W=17.62 Since both the GSC2 and GALEX coverage of the field of view is poor in terms of limiting magnitude, and following the recommendation of Sect. 10.4.1 of COS-instrument handbook, we queried UV photometry from program GO-16104 to check whether the targets are clear from Unsafe objects within a 43'' diameter circle. The brightest source found has F225W=16.94, F275W=17.23. This target is Sextans-A-OB523 that was safely observed with COS-G140L in program GO-14245 and with COS-G130M in GO-15880. Nonetheless we checked this source in the ETC with the following parameters: Unreddened Kurucz models for O5V stars High settings for airglow lines and zodiacal light, and extremely high for Earth shine. EXPTIME=2700s for spectroscopy, EXPTIME=10s for ACQ/IMH The count rate did not exceed the recommended values in any case. COS2025 ------- Observations with the G140L gratings are unaffected by the COS2025 policies. IMPACT OF REDUCED GYRO MODE --------------------------- The impact of 2-gyro operations on these observations would be limited since: - The observations are not time critical in any way. - No ORIENT constraints have been requested. - We have arranged the exposures in visits of 3 orbits or less to facilitate scheduling. - Accuracy of pointing is not critical as long as the observatory can ensure that the initial pointing of COS-NUV-ACQ/IMAGE already locates targets within the PSA, and that the COS-ACQ/IMAGE warrants centering the target with the required accuracy. Other points that would impact our program (but just as any other program): - Failed acquisitions, or increased target acquisition time that would reduce the net science exposure time per orbit. REMAINING WARNINGS ---------------------------------- The proposal contains warnings regarding the mandatory use of all FFPOS. Some orbits use only 2 FPPOS, but we arranged the observations to make a balanced use of all 4 FPPOS. The PI M. Garcia has led 2 HST-COS proposals (GO-12587, GO-14245) on the topic of UV spectroscopy of massive stars in the Local Group. Both were carried out successfully. After completion, the ETC-estimated UV fluxes at 1500\AA were checked to be very close to the actual observed fluxes, which endorses the methodology used to compute exposure times and ensures COS safety. The current proposal builds on the team's experience after GO-12587 and GO-14245. It requests UV spectroscopy of a selection of OB-type stars in Sextans A unveiled by optical spectroscopy. The broader sample, built after 5 observing runs with the 10m telescope GTC, constitutes the only extensive collection of 1/10 Zsun resolved massive stars available world-wide. A comprehensive paper by graduate student M. Lorenzo presenting the ground-based optical spectra is in preparation. All co-authors have ample experience in UV spectroscopy and/or massive stars. J.Roman-Duval is the Lead of the Core Implementation Team of ULLYSES's DDT program, and A. Fullerton is the Lead Expert on High Mass Stars. Danniel Lennon is a former COS team member and has lead numerous proposals to observe massive stars with HST. Co-I's N. Castro, C. J. Evans, A. Herrero and M. A. Urbaneja have a long record of studies of extragalactic massive stars. Co-I Najarro is expert user and developer of the CMFGEN code, that will be used to analyze the observed UV spectra. A. Wofford's expertise is spectroscopic observations and analysis of unresolved massive-star clusters, star forming galaxies, and starburst galaxies. She has led several HST-COS observational campains targeting metal-poor star-forming dwarf galaxies and massive star clusters (GO-13788, GO-15220, GO-15828 and GO-16175), and multiple studies of nearby star-forming regions involving UV and optical imaging and spectroscopy with HST STIS, COS, ACS, and WFC3. The team's ample experience in handling and analyzing UV data is endorsed by multiple publications, e.g.: - Wofford, A., et al. 2021, MNRAS, 500, 2908 - Garcia, M., Herrero, A., Najarro, F., Lennon, D.J., Alejandro Urbaneja, M., 2014, ApJ, 788, 64 - Lennon, D., et al., 2010, Instrument Science Report COS 2010-07(v1) - Garcia, M., & Bianchi, L., 2004, ApJ, 606, 497 - Evans, C.J., Crowther, P.A., Fullerton, A.W. & Hillier, D .J. 2004, ApJ, 610,1021 - Urbaneja,M.A., Herrero, A., et al. 2002, A&A, 386, 1019 - Herrero, A., et al., 2001, A&A, 366, 623 Stellar Physics and Stellar Types Galaxies 6 false false true false false false false SUPPORTED EXT-STAR MAIN SEQUENCE O NO J101105.28-044238.3 LGN-S002 J2000 J2000 B-V=-0.279; E(B-V)=0.023; SpT=O5Vz; WFC3/UVIS-F225W=17.87; F_1300=1.6E-15 erg/cm2/s/A EXT-STAR MAIN SEQUENCE O NO J101106.48-044237.1 LGN-S007 J2000 J2000 B-V=-0.28; E(B-V)=0.031; SpT=O6V; WFC3/UVIS-F225W= 17.93 ; F_1300=1.4E-15 erg/cm2/s/A EXT-STAR GIANT O NO J101103.70-044234.2 LGN-S011 J2000 J2000 B-V=-0.22; E(B-V)=0.108; SpT=O7.5III; WFC3/UVIS-F275W=17.97; F_1300=1.3E-15 erg/cm2/s/A EXT-STAR SUPERGIANT O NO J101105.30-044210.1 LGN-S049 J2000 J2000 B-V=-0.268; E(B-V)=0.031; SpT=O9.7I; WFC3/UVIS-F225W=17.58; F_1300=1.8E-15 erg/cm2/s/A 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 /home/mgg/MGG/scratch/proposals/HST/2022/LOWZ/PHASE2/APT/OP-cache/v0-v01.xml The scheduling data was generated by CASM 30.3. 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CASM was run in Phase II mode. (Tic-Visit :proposal-id 17111 :visit-id "10" :proposal-version -1 :trans-version "20220516" :date "14-Jul-2022 18:37:03.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 121952 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17111 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17111 :visit-id "10" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2749 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17111 :visit-id "10" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2750 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17111 :visit-id "10" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2750 :al-overhead-at-end 0 :internal-dur-at-end 363 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 3 0 /home/mgg/MGG/scratch/proposals/HST/2022/LOWZ/PHASE2/APT/OP-cache/v0-v11.xml The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17111 :visit-id "11" :proposal-version -1 :trans-version "20220516" :date "14-Jul-2022 18:37:04.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 78400 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17111 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17111 :visit-id "11" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2749 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17111 :visit-id "11" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2750 :al-overhead-at-end 0 :internal-dur-at-end 363 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 2 0 /home/mgg/MGG/scratch/proposals/HST/2022/LOWZ/PHASE2/APT/OP-cache/v0-v12.xml The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17111 :visit-id "12" :proposal-version -1 :trans-version "20220516" :date "14-Jul-2022 18:37:04.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 78400 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17111 :visit-id "12" :obset-id "12" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17111 :visit-id "12" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2749 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17111 :visit-id "12" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2750 :al-overhead-at-end 0 :internal-dur-at-end 363 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 2 0