Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.0Assigned ID: 3821
----- Attempting Submission 1 (Wed Oct 19 17:32:46 GMT 2022) -----
HST Phase I Proposal 3821 successfully submitted.
Receipt: # 3821-1
----- Attempting Submission 2 (Thu Oct 20 20:20:16 GMT 2022) -----correct lifetime position for the G160M were varified in manualFor 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.
COS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS
INEFFICIENT ORDERING OF FP-POS POSITIONS
COS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS0----- Attempting Submission 1 (Thu Dec 15 18:09:43 GMT 2022) -----1. Exposure time rounding verified
2. FP-POS positions for exposure 3 + 4 adjusted to FP-POS=3,4 based on guidelines in COS manual (to the best of my understanding)
3. I don't understand the remark regarding decreasing FP-POS values; to me, it seems like the values are increasing from exposure 3 to exposure 4.Benchmarking the first bona fide extragalactic X-ray faint massive black-hole binaryWe propose to secure two phase-resolved HST/COS UV spectra of VFTS 243: the only known X-ray faint binary hosting a black hole outside our Milky Way. VFTS 243, a 10-d period binary residing in the Large Magellanic Cloud, was recently reported (July 2022, Nature Astronomy) to comprise a 25Msun O-type primary and a black hole that weighs at least 9Msun. Unlike all other extragalactic black holes known, the black hole in VFTS 243 is X-ray quiet. VFTS 243, which received wide media coverage, thus provides us with a laboratory to study black hole formation, supernova physics, and wind accretion in an uncharted parameter domain. With only two orbits of UV spectroscopy, we will: (1) establish the wind properties of the O-type primary, which is crucial for understanding the lack of X-rays in the system; (2) ensure that no hot companion is hidden in the spectrum; (3) investigate whether the atmosphere of the primary is polluted by material from a previous mass-transfer or explosion event, and (4) study the interaction between the black hole and the stellar wind in an X-ray faint black hole binary. These investigations will shed light on the formation process of black holes at sub-solar metallicity and on accretion physics, with implications on gravitational-wave astronomy and supernova physics.We aim to obtain UV spectra with the G130M (1222 & 1291) and G160M(1623) gratings of the O+black-hole binary VFTS 243 at two distinct orbital phases:
- Phase ~0.32 or ~0.82 (RV extreme)
- Phase ~0.07 (black hole in front of O star)
The spectra should cover the range ~1100-1800Ang, with an S/N of 5-10 in @ 1500Ang per resolution element.Tomer Shenar (PI), Hugues Sana, & Laurent Mahy are experts for spectroscopy of massive binaries in the UV, optical, and infra-red, with ample experience in OB-type stars and helium stars. They also maintain (and co-develop) non-LTE modelling tools such as PoWR, CMFGEN, and FASTWIND. Tomer Shenar, Kareem El-Badry & Julia Bodensteiner have unparalleled experience in investigating OB+BH candidates. Norbert Langer & Pablo Marchant are renowned experts in binary evolution.Stellar Physics and Stellar Types3falsefalsetruefalsefalsetruefalsefalseSUPPORTEDEXT-STARMAIN SEQUENCE ONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000UIT_B1 flux [cgs/A]= 8.79E-15 @ lam =1521 AngCOS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1623The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.Visit at RV extreme, phases 0.32 or 0.82.
Current time requirement set for phase interval 0.72 - 0.92 (RV extreme is at ~0.82)
However, the interval 0.22 - 0.42 would work equally well.1686972008000180.40852240762263(Tic-Visit
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)false10ETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Model already includes extinction (EBV = 0.55 for RV=3.1; AV=1.7; Shenar+22), hence EBV=0 in ETC run.ETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Model already includes extinction (EBV = 0.55 for RV=3.1; AV=1.7; Shenar+22), hence EBV=0 in ETC run.
ExpTime ~ 370/4 ~ 90sec per subexposure for S/N ~5 at 1300AngETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Adopted extinction: EBV = 0.54 (at RV=3.1)
ExpTime ~ 400/2 sec for S/N ~5 at 1350Ang
Split into FP-POS 3 & 4 (exposures 3 & 4)ETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Adopted extinction: EBV = 0.54 (at RV=3.1)
ExpTime ~ 400/2 sec for S/N ~5 at 1350Ang
Split into FP-POS 3 & 4 (exposures 3 & 4)ETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Model already includes extinction (EBV = 0.55 for RV=3.1; AV=1.7; Shenar+22), hence EBV=0 in ETC run.
ExpTime ~ 370/4 ~ 90sec per subexposure for S/N ~5 at 1500AngThe scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.Visit at conjunction, black hole in front of primary (phi = 0.0645)1686162451000172.7(Tic-Visit
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)false10ETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Model already includes extinction (EBV = 0.55 for RV=3.1; AV=1.7; Shenar+22), hence EBV=0 in ETC run.ETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Model already includes extinction (EBV = 0.55 for RV=3.1; AV=1.7; Shenar+22), hence EBV=0 in ETC run.
ExpTime ~ 370/4 ~ 90sec per subexposure for S/N ~5 at 1300AngETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Adopted extinction: EBV = 0.54 (at RV=3.1)
ExpTime ~ 400/2 sec for S/N ~5 at 1350Ang
Split into FP-POS 3 & 4 (exposures 3 & 4)ETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Adopted extinction: EBV = 0.54 (at RV=3.1)
ExpTime ~ 400/2 sec for S/N ~5 at 1350Ang
Split into FP-POS 3 & 4 (exposures 3 & 4)ETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Model already includes extinction (EBV = 0.55 for RV=3.1; AV=1.7; Shenar+22), hence EBV=0 in ETC run.
ExpTime ~ 370/4 ~ 90sec per subexposure for S/N ~5 at 1500AngThe scheduling data was generated by CASM 31.0.CASM was run in Phase II mode./System/Volumes/Data/solaris/user1/royle/OP-cache/17279-v03.xmlVisit at conjunction, black hole in front of primary (phi = 0.0645)(Tic-Visit
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Model already includes extinction (EBV = 0.55 for RV=3.1; AV=1.7; Shenar+22), hence EBV=0 in ETC run.ETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Model already includes extinction (EBV = 0.55 for RV=3.1; AV=1.7; Shenar+22), hence EBV=0 in ETC run.
ExpTime ~ 370/4 ~ 90sec per subexposure for S/N ~5 at 1300AngETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Adopted extinction: EBV = 0.54 (at RV=3.1)
ExpTime ~ 400/2 sec for S/N ~5 at 1350Ang
Split into FP-POS 3 & 4 (exposures 3 & 4)ETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Adopted extinction: EBV = 0.54 (at RV=3.1)
ExpTime ~ 400/2 sec for S/N ~5 at 1350Ang
Split into FP-POS 3 & 4 (exposures 3 & 4)ETC input: tailored model atmosphere for VFTS 243 (from Shenar et al. 2022, Nat As, 2022, 6, 1085, calculated with PoWR code.
Model already includes extinction (EBV = 0.55 for RV=3.1; AV=1.7; Shenar+22), hence EBV=0 in ETC run.
ExpTime ~ 370/4 ~ 90sec per subexposure for S/N ~5 at 1500Ang