0Assigned ID: 306
----- Attempting Submission 1 (Fri Apr 05 00:36:29 GMT 2019) -----
HST Phase I Proposal 306 (wn3-uv.APT.apt) successfully submitted.
Receipt: # 306-1
----- Attempting Submission 2 (Fri Apr 05 21:05:30 GMT 2019) -----added spectral acquisition for visits 1-7, 10 and new ETC calcualtions for these.-1209487531----- Attempting Submission 1 (Fri Jul 19 21:46:38 GMT 2019) -----
----- Attempting Submission 2 (Fri May 01 20:28:35 GMT 2020) -----Orbit planner and visit planner can't be run for visits 8 & 9 - already in scheduling.UV spectroscopy of He stars: the elusive stripped-envelope supernova progenitorsWe propose to obtain UV spectra of 10 stars in the LMC that represent a new subtype of Wolf-Rayet (WR) star. These stars, classified as WN3/O3 stars, were identified in a recent narrow-band survey. They represent a major puzzle because they are less luminous and hotter than traditional WR stars, which models usually explain by either wind mass-loss or rapid rotation, yet their winds are very weak. These WN3/O3 stars may be examples of the long-sought He stars at relatively low initial mass (10-20 Msun) that have had their H envelopes stripped in binary systems. This explanation may be favored because (1) their locations are far from O-type stars, requiring long lifetimes and low initial masses of 10-20 Msun, and (2) their spectra and approximate locus on the HR diagram are matched well by stripped binary models. Such binary He stars are extremely important: they have become leading candidates for the progenitors of stripped-envelope supernovae (SNe with no H), they are candidate progenitors of kilonovae/NS+NS mergers, and they may play a critical role in cosmic reionization. Even though they should be quite common, they are elusive because they are too hot and faint to detect in visual photometry nearby galaxies, and they are hard to see locally because their mass-gainer secondary star usually outshines them. If they are binaries, these particular 10 stars are readily observable because they may have low-mass main-sequence companions that did not accrete much mass. Space-based UV spectroscopy can tightly constrain their fundamental parameters. - especially their mass-loss rates, which regulate their escaping ionizing photons, and help determine their eventual fate.This program will obtain UV spectra for 10 targets in the LMC that are a class of Wolf-Rayet stars called WN3/O3 stars, which exhibit both wind emission lines of WR stars but also absorption lines of hot O-type atmospheres. The goal is to obtain UV spectra and SEDs that can be modeled to more tightly constrain the physical parameters of the stars. Spectra will be obtained in the FUV G160M setting, centered on 1577 AA, with the maximum expore time available in one CVZ orbit per star using all 4 FP positions.All investigators on this proposal are experts in various aspects of massive star evolution. Dr. Selma de Mink is an expert on theoretical studies of a wide range of problems in massive binary star evolution, mass transfer and stellar mergers, binary vs. single star population synthesis, and a variety of implications for observational studies of massive stars. Dr. Jose Groh conducts both observational and theoretical studies of massive stars, and the impact of mass loss on their evolution. This includes stellar evolution models, and CMFGEN radiative transfer models to derive accurate physical properties of stars, their wind mass loss, and radiative transfer models of supernova explosions. Dr. Ylva Gotberg is an expert in theoretical studies using stellar evolution models and radiative transfer models to investigate products of mass stripping in close binary evolution, their predicted observational signatures, and their contribution to the radiation budget of stellar populations. Dr. Maria Drout is an expert in observational studies of evolved cool supergiants in nearby galaxies, a wide range of supernova explosions, and other transients including kilonovae. These studies of transients include a particular emphasis on supernovae that have experienced significant mass stripping. Dr. Nathan Smith concentrates on observational studies of mass loss from massive stars, including winds, eruptions, and binary mass loss, implications for the late evolution of massive stars and stellar populations, and studies of supernovae from massive stars with significant mass loss.Stellar Physics6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARWOLF RAYETNOJ2000J2000STARWOLF RAYETNOJ2000J2000STARWOLF RAYETNOJ2000J2000STARWOLF RAYETNOJ2000J2000STARWOLF RAYETNOJ2000J2000STARWOLF RAYETNOJ2000J2000STARWOLF RAYETNOJ2000J2000STARWOLF RAYETNOJ2000J2000STARWOLF RAYETNOJ2000J2000STARWOLF RAYETNOJ2000J2000COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode.(Tic-Visit
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