Final submission, hopefully!892962205Assigned ID: 293
----- Attempting Submission 1 (Thu Apr 07 21:25:17 GMT 2016) -----
HST Phase I Proposal 293 (apt_onfp_c24_v1.pdf.apt) successfully submitted.
Receipt: # 293-1
----- Attempting Submission 2 (Fri Apr 08 07:40:14 GMT 2016) -----
HST Phase I Proposal 293 (apt_onfp_c24_v1.pdf.apt) successfully submitted.
Receipt: # 293-2
----- Attempting Submission 3 (Fri Apr 08 12:03:18 GMT 2016) -----0For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
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.
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.10/25/2016: phase II resubmittted with revised ACQs for Visits 1-3.712873836----- Attempting Submission 1 (Mon Jul 18 20:15:11 GMT 2016) -----
HST Phase II Proposal 14683 (jcb_phase2_v6.apt.2016_07_14_09_55.aptbackup.2016_07_14_16_14.aptbackup.2016_07_14_16_17.aptbackup.2016_07_14_20_33.aptbackup.2016_07_18_15_23.aptbackup) successfully submitted.
Receipt: # 14683-1
----- Attempting Submission 2 (Mon Jul 18 20:16:33 GMT 2016) -----
HST Phase II Proposal 14683 (jcb_phase2_v6.apt.2016_07_14_09_55.aptbackup.2016_07_14_16_14.aptbackup.2016_07_14_16_17.aptbackup.2016_07_14_20_33.aptbackup.2016_07_18_15_23.aptbackup) successfully submitted.
Receipt: # 14683-2
----- Attempting Submission 3 (Wed Jul 20 21:40:41 GMT 2016) -----
HST Phase II Proposal 14683 (jcb_phase2_v6.apt.2016_07_14_09_55.aptbackup.2016_07_14_16_14.aptbackup.2016_07_14_16_17.aptbackup.2016_07_14_20_33.aptbackup.2016_07_18_15_23.aptbackup.2016_07_19_15_35.aptbackup.2016_07_19_20_02.aptbackup) successfully submitted.
Receipt: # 14683-3
----- Attempting Submission 4 (Tue Oct 25 13:12:43 GMT 2016) -----Hi, As you will see, the three stars that we want to observe with COS will use 2 FP-POSs only. Our COS reviewer told us that even though that doesn't officially meet the goal of using FP-POS=ALL, it meets the spirit of spreading the damage from airglow around the detector and allowing for the
correction of fixed pattern noise.Before the Burst: The Properties of Rapidly Rotating, Massive SupergiantsRapidly rotating, evolved massive stars are thought to be the progenitors of long gamma-ray bursts (LGRBs). Their rapid rotation may be the result of (a) reduced angular-momentum loss by a single star due to reduced mass loss at low metallicity; or (b) spin-up via mass and angular momentum transfer from a companion or a stellar merger. Independent of their formation mechanism, the properties of their stellar winds are strongly affected by their rapid rotation. We have recently obtained optical spectroscopy to study the properties of a sample of ten fast rotating, evolved massive stars in the Large Magellanic Cloud. Here, we propose to use HST FUV spectroscopy to determine the wind properties of these objects. The information needed to characterize the stellar winds of massive stars is encoded in FUV spectra. Establishing the properties of these rotating outflows is a critical issue, since the present uncertainties restrict our understanding of the evolution of the angular momentum, the initial-to-final mass relation, and the ultimate fate of a massive star.
By fitting line profiles from sophisticated model atmospheres to the FUV spectra, we will measure photospheric CNO abundances, probe the rotation law of the stellar wind, and study the influence of rapid rotation on the profiles of wind lines, and hence on the determination of mass-loss rates. We will investigate how rapid rotation affects the onset of clumping, the presence of which reduces estimates of mass-loss rates. This program will enable decisive steps toward determining the nature of rapidly rotating, evolved, massive stars, as required to evaluate their suitability as progenitors of LGRBs.Here, we propose to use HST FUV spectroscopy to determine the wind properties of rapidly rotating, evolved massive stars in the Large Magellanic Cloud. The information needed to characterize the stellar winds of massive stars is encoded in FUV spectra. Wind terminal velocities will be measured from the blue edge of absorption component of P Cygni profiles. Mass-loss rates will be derived from P Cygni profiles from resonance doublets of N v 1238-1242, Si iv 1393-1402, and C iv 1548-1550. Excited state wind lines are also available, and provide different sensitivities to density and the radiation field from resonance transitions (e.g. He ii 1640). Clumping parameters can be derived from O v 1371 and N iv 1718 but also He ii 1640 which is very sensitive to clumping for stars with strong winds.
For five of the selected targets, we choose to use STIS in the E140M setting, because it provides spectra over the entire wavelength range (1150-1700 A) in a single exposure, with low overheads. ACCUM mode was selected because we don't need/want high time resolution. These stars are bright and/or have low E(B-V). Our nominal target signal-to-noise ratio (SNR) is ~ 15-20 per resolution element, sufficient to measure the weakest CNO lines used for abundance analyses for instance. Exposure times were determined with the STIS ETC by scaling early to mid-O star Kurucz templates to the observed V magnitude. We used the LMC diffuse extinction curve and E(B-V) computed from the photometry and intrinsic colors to redden the spectrum. For targets in the LMC, the visibility is 60 min per orbit. Allowing for guide-star and target acquisitions (6mn for first exposure, 4mn for reacquisition) and instrument overhead (2-4 min), we should typically have about 50-55 min of spectroscopic exposure. Using this input, we find that a single non-CVZ orbit will give a SNR ~15-20 per resolution element at 1600 A in one orbit for 1 target. For two stars, 2 orbits are needed to reach this SNR, and two other stars require 3 orbits.
For three stars, we shall take advantage of the higher FUV sensitivity, in the G130M (settings 1291, 1327) and G160M (1577, 1623) gratings, for the maximum, uninterrupted wavelength coverage of 1134-1798 A. The resolving power of these settings (R ~ 20,000) is optimal for wind and photospheric parameters characterization (e.g. surface abundances). Exposure times were determined with the COS ETC with the same template as for STIS (above). The required SNR (~20) can be achieved in a single orbit for these stars, using 2 FP-POS for each central wavelength. It will be further improved by co-adding overlapping segments. For targets in the MCs, the visibility is 60 min per orbit. Guide star acquisition consumes 6 min and COS imaging target acquisition (supported by our accurate coordinates and elimination of excessively crowded targets) another 3 min. COS overheads for the required 4-setting sequence are 5+2+3+2=12 min, so that total overheads amount to 21 min, leaving 39 min of spectroscopic exposure time. For a typical 1:2 ratio between the two gratings, that reduces to 13 min (780 sec) for G130M and 26 min (1560 sec) for G160M.Stellar Physics6falsetruefalsefalsefalsefalseAVAILABLEEXT-STAREMISSION LINE STAROFSUPERGIANT OWINDNOJ2000J2000B-V= 0.10, O2 - 3(n)f*pEXT-STAREMISSION LINE STAROFSUPERGIANT OWINDNOJ2000J2000B-V=-0.12, O7.5n(f)pEXT-STAREMISSION LINE STAROFSUPERGIANT OWINDNOJ2000J2000B-V=-0.18, O6n(f)pEXT-STAREMISSION LINE STAROFSUPERGIANT OWINDNOJ2000J2000B-V=-0.15, O6.5(n)(f)pEXT-STAREMISSION LINE STAROFSUPERGIANT OWINDNOJ2000J2000B-V=-0.22, O5n IfpEXT-STAREMISSION LINE STAROFSUPERGIANT OWINDNOJ2000J2000B-V=-0.15, O5n(f)pEXT-STAREMISSION LINE STAROFSUPERGIANT OWINDNOJ2000J2000B-V=-0.03, O5n(f)pEXT-STAREMISSION LINE STAROFSUPERGIANT OWINDNOJ2000J2000B-V=-0.18, O7.5(n)(f)pCOS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1623STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1623STIS/FUV-MAMASpectroscopicNoNoE140M1425COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1623STIS/FUV-MAMASpectroscopicNoNoE140M1425The scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.1492575255000123.89449805194482(Tic-Visit
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