0Assigned ID: 4775
----- Attempting Submission 1 (Wed May 24 22:54:42 GMT 2023) -----
HST Phase I Proposal 4775 successfully submitted.
Receipt: # 4775-1
----- Attempting Submission 2 (Wed May 24 23:44:38 GMT 2023) -----ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN07/30/2024 Added visit #55 to replace failed visit #05.
Detected errors refer to already completed visits.
12/29/2023 Corrected errors in the ACQ ETC reference numbers.
These are UV bright targets, but STIS ETC estimates show safe observations are possible
with appropriate ND filters.
Note that the second "v2" visit for each target is to be scheduled near a binary conjunction;
one is selected under Special Requirements and the other conjunction is mentioned in
the Comments block.
Comments apply to this Phase II submission (09/14/2023).297549616----- Attempting Submission 1 (Thu Sep 14 15:48:07 GMT 2023) -----
----- Attempting Submission 2 (Fri Dec 29 18:35:21 GMT 2023) -----
----- Attempting Submission 3 (Tue Jul 30 17:26:00 GMT 2024) -----Errors refer to completed visits.Masses of Be+sdO binaries with visual orbitsMassive stars are often created in close binary systems that are destined to exchange mass and angular momentum. The more massive component will begin transferring photospheric gas to its companion when it attains a physical size becomes comparable to its Roche surface. The mass donor will eventually be stripped of its outer envelope to become a hot He star, and the mass gainer will be spun up to near critical rotation. The rapidly rotating Be stars may have formed through such close binary interaction, and a large fraction of them may exist as Be+He binaries, which have been called Be+sdO systems in published research papers. Searches for the hot He stars are only feasible with ultraviolet spectroscopy. Here we propose to obtain FUV spectroscopic observations for five Be+sdO binaries systems that were recently angularly resolved through near-IR long baseline interferometry with the CHARA Array. The visual orbits combined with distances yield the total system masses, but to obtain individual masses requires spectroscopic orbits from radial velocities. Our goals here are to confirm the detection of the stripped helium stars in these Be binaries, determine their orbital elements through measurements of the Doppler shifts, find the individual masses, and refine the physical properties of both components from the reconstruction of individual component spectra using Doppler tomography. We aim to compare the fundamental physical parameters of these systems with evolutionary models to estimate their ages and to trace their formation processes through the mass transfer.We propose to obtain high dispersion, FUV spectroscopic observations of five Be+sdO binary systems that are directly resolved through interferometric observations. The FUV observations will be made with HST/STIS in a configuration that covers the spectral range of 1150-1710 Angstroms using the E140M grating and MAMA detector. This wavelength range and spectral resolution are needed to detect the signal of the stripped helium stars.
All the targets have 54 to 61 minutes of visibility in each orbit. By deducting 6 minutes for guide star acquisition, 6 minutes for STIS target acquisition, 6 minutes for target peak-up, and 8 minutes for STIS overhead science observations, there remains 29 minutes (1740 seconds) science exposure time in one orbit. We used the HST/STIS exposure time calculator (ETC) and the existing IUE spectra of three targets to determine the net spectral signal-to-noise ratio (S/N). For the two targets without IUE spectra, HD 161306 and 7 Vul, we adopted model spectra associated with the Be and sdO stars that were fit to published photometry and TD1 UV fluxes. A S/N > 40 per resolution element is achieved for each target for the integration time available in one orbit. Because all the targets are bright in the UV, a neutral density filter is selected for each target (except in the case of HD 161306) to avoid exceeding the bright limit of the MAMA detector.
We request three visits to each target (a total of 15 visits) to confirm the detection of the subdwarf in the Be binary systems and measure the subdwarf radial velocities. Based on the well-determined orbital periods from prior spectroscopic studies, we plan to schedule the first and second visits near the two orbital quadrature phases and the third visit near a conjunction phase (+/-10% phase interval). One conjunction phase is set in the "v2" visit, but the second conjunction phase is also acceptable (see Comments block for v2). This phase distribution will record the extreme and middle Doppler shifts of each stellar component, and this is sufficient to determine the mass ratio and perform the Doppler tomography reconstruction of the spectra).Dr. Douglas Gies is a long-time practitioner studying massive binary stars, and he has led several HST investigations of spectroscopic binaries. Dr. Luqian Wang has experience analyzing the Be+He binaries using both ground-based and space UV spectroscopy. Dr. Geraldine Peters is an expert in space observations of hot stars and has led many important investigations on the Be binaries. Dr. Robert Klement has expertise in observing and analyzing the Be binaries using near IR interferometric and radio data.Stellar Physics and Stellar Types6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARB0-B2 V-IVBENOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates from Gaia EDR3.HR-2142J2000J2000F(1425) = 4.1e-10 erg/s/cm^2/AngstromSTARB6-B9.5 III-IBENOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates from Gaia EDR3.HD-109387HR-4787J2000J2000F(1425) = 8.1e-10 erg/s/cm^2/AngstromSTARB3-B5 V-IVBENOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates from Gaia EDR3.MWC-271J2000J2000F(1425) = 1.71e-12 erg/s/cm^2/AngstromSTARB3-B5 V-IVBENOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates from Gaia EDR3.HD-183537HR-7409J2000J2000F(1425) = 8.5e-11 erg/s/cm^2/AngstromSTARB0-B2 V-IVBENOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates from Gaia EDR3.HD-200310HR-8053J2000J2000F(1425) = 6.4e-10 erg/s/cm^2/AngstromSTIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/FUV-MAMASpectroscopicNoNoE140M1425The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode./private/var/folders/m2/fmjhy30n135bdth71j_lyvfh0000gn/T/OPVisit14175798084414019836.xml170989681400080.69999999999999(Tic-Visit
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