0Assigned ID: 375
----- Attempting Submission 1 (Fri Apr 11 05:55:08 GMT 2014) -----
HST Phase I Proposal 375 (vfts352.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 15:48:26 GMT 2014) -----For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
If the target coordinates are not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE.Identical as previous submission but the individual exposure have been split accross 2 FP-POS in each visit.1660481366----- Attempting Submission 2 (Thu Jul 24 01:57:42 GMT 2014) ------ 2 FP-POS are used in each visit (1 orbit per visit). All 4 FP-POS are equally used throughout the 8 visit towards the target.
- the star coordinate are from GSC2.3 ( S0U9127185) are are thus believed to be accurate to within 0.3"UV spectroscopy of the most massive overcontact binary known to date: on the verge of coalescence ?Binary interaction dominates the evolution of massive stars. Because of the abundance of short period systems, about a quarter of all massive stars are thought to merge with their companion. The short-lived contact phase preceding coalescence is poorly understood due to the lack of observational constraints: only two overcontact O-type binaries are known so far. Yet, these systems provide crucial observational testbeds to understand the elusive formation and evolution of the most massive stars, the complex physics of stellar mergers and the role that the coalescence products play as progenitors of supernovae and gamma-ray bursts. We recently discovered VFTS 352, the most massive, earliest spectral type and shortest period (P = 1.12 d) overcontact O-type binary known to date. With an estimated combined mass of 130 Msun, this truly unique system is expected to merge into a rapidly rotating, very massive, single star. Initial estimates of the physical parameters were derived from high-quality ground-based optical spectra and photometry. Yet, optical analyses of overcontact systems can overestimate the radial-velocity amplitudes, hence the masses, by up to 40% because optical lines are susceptible to irradiation effects. Here we propose a limited 8-epochs COS monitoring of VFTS 352. The G130M and G160M spectra will allow us to side step the uncertainties affecting optical determination of the masses and to constrain the mass loss rate and CNO surface abundances. These constraints are crucial to identify the complex mixing processes, to reveal signs of mass exchange and mass loss from the system, and to enable a comparison with massive binary evolution models.We perform G130m/1291 and G160M/1611 COS FUV spectroscopy of the same object at 8 different orbital phase (exposure centered on phases 0.0, 0.125, 0.25, 0.375, 0.5, 0.625, 0.75 and 0.875). Kind request that all observations are done within 2 weeks and at the same LP position.HOT STARSDefaultfalsetruefalsefalsefalseSUPPORTEDSTARMAIN SEQUENCE OJ2000J2000F275W = 13.3magCOS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1291/home/hsana/Dropbox/PROPOSAL/HST/C22/VFTS352/APT/OP-cache/vfts352_Jul22_2FP-POS-v01.xmlTiming link suitability includes constraints ([Group (01 02 03 04 05 06 07 08) Within 12.0 days])The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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