0Assigned ID: 1843
----- Attempting Submission 1 (Fri Apr 09 07:21:40 GMT 2021) -----
HST Phase I Proposal 1843 successfully submitted.
Receipt: # 1843-1
----- Attempting Submission 2 (Fri Apr 09 21:04:26 GMT 2021) -----
HST Phase I Proposal 1843 successfully submitted.
Receipt: # 1843-2We have updated so MirrorB is used on all acquisitions.511251979----- Attempting Submission 1 (Thu Jul 29 16:35:15 GMT 2021) -----
HST Phase II Proposal 16755 successfully submitted.
Receipt: # 16755-1
----- Attempting Submission 2 (Fri Nov 19 20:05:03 GMT 2021) -----The target confirmation chart program was run.
However, for 5/7 sources in my program the tool failed to properly generate the PDF.
The various component images *were* all generated in my directory (e.g. the dss fits file, a wide-field png, and a zoomed png all appear).
However, instead of compiling into a PDF, the APT hung, stopped responsing, and eventually I had to force quit and reopen.
I have examined the pngs directly.From Supernova Progenitors to Ionizing Radiation - HST/COS Spectroscopy of Stripped Helium StarsBinary population synthesis models predict that ~30% of massive stars will have their hydrogen envelopes removed via interaction with a binary companion. The resulting ``stripped'' helium cores are relatively long-lived, hot, compact, and emit extreme ultraviolet radiation. As a result, they represent a critical piece in our understanding of the ionizing radiation from stellar populations as well as the nature of supernova and gravitational wave progenitors. However, despite their importance and predicted ubiquity, observations have remained elusive. This is now changing. Using UV maps of the Magellanic Clouds, a sample of candidate systems has been identified. Optical spectroscopy reveals stars with temperatures in excess of 60,000 K, but luminosities intermediate between Wolf-Rayet and subdwarf stars. A lack of strong emission line features indicates their mass loss rates must be more than an order of magnitude lower than previously assumed based on extrapolations from higher luminosity stars. Here, we propose to obtain HST/COS spectra of a sample of 7 of these helium stars in the Magellanic Clouds. UV observations are necessary to measure their mass loss and wind parameters, and this sample was chosen to allow the first observational constraints of these parameters as a function of both luminosity and metallicity. Precise mass loss parameters will have a large impact on the stellar radii, ionizing radiation, and final surface composition of stripped helium stars. These HST/COS observations will therefore provide vital constraints for models of binary evolution, impacting our understanding of supernova progenitors, gravitational wave sources, and ionizing radiation.This program will obtain UV spectra for 7 targets in the LMC/SMC that are newly discovered intermediate mass stripped helium star candididates. These are hot stars that are more luminous than subdwarfs, but lack the wind emission lines of Wolf-Rayet stars. The goal is to obtain UV spectra that can be modeled to constrain their wind parameters and other physical properties. Spectra will be obtained in the FUV with the G140L grism and a center wavelength of 800 AA, providing continuous wavelength coverage between ~900-1950 AA. We use the maximum exposure time avalible in between 1-3 orbits allocated per star, using all four FP positions for each target.
The impacts of a reduced gyro operations on this program would primarily be reduced schedualability due to the smaller field of regard, as well as possible impacts of roll angle constraints when avoiding placement of bright field objects in the second COS aperture. Slightly longer acquisition times would have only a small effect on the S/N of our observations.All investigators on this proposal are experts in various aspects of massive star evolution.
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. Bethany Ludwig is a PhD student at the University of Toronto and expert at UV phototmetry in crowded stellar regions. 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. Eoin Farrell is a PhD student at Trinity College Dublin and an expert in stellar structure modelling of post main sequence stars. 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. Dr. Maria Drout is an expert in observational studies of evolved stellar populations 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.Stellar Physics and Stellar TypesStellar Populations and the Interstellar Medium6falsefalsetruefalsefalsefalsefalseSUPPORTEDEXT-STARCOMPOSITE SPECTRAL TYPESDOWOLF RAYETNOJ2000J2000UVW2: 17.30 mag (AB), UVM2: 17.56 mag (AB)EXT-STARCOMPOSITE SPECTRAL TYPESDOWOLF RAYETNOJ2000J2000UVW2: 17.73 mag (AB), UVM2: 17.80 mag (AB)EXT-STARCOMPOSITE SPECTRAL TYPESDOWOLF RAYETNOJ2000J2000UVW2: 17.86 mag (AB), UVM2: 17.97 mag (AB)EXT-STARCOMPOSITE SPECTRAL TYPESDOWOLF RAYETNOJ2000J2000UVW2: 18.16 mag (AB), UVM2: 18.27 mag (AB)EXT-STARCOMPOSITE SPECTRAL TYPESDOWOLF RAYETNOJ2000J2000UVW2: 16.18 mag (AB), UVM2: 16.26 mag (AB)EXT-STARCOMPOSITE SPECTRAL TYPESDOWOLF RAYETNOJ2000J2000UVW2: 17.94 mag (AB); UVM2: 17.98 mag (AB)EXT-STARCOMPOSITE SPECTRAL TYPESDOWOLF RAYETNOJ2000J2000UVW2: 17.82 mag (AB), UVM2: 17.88 mag (AB)COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.(Tic-Visit
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