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Assigned ID: 434
----- Attempting Submission 1 (Fri Mar 06 09:58:28 GMT 2020) -----
As per HOPR 92154, we have copied 2 orbits from Visit 02 to be repeated as Visit 17 and 2 orbits from Visit 09 to be repeated as Visit 18
1289187150
----- Attempting Submission 1 (Fri Jun 05 14:57:28 GMT 2020) -----
HST Phase II Proposal 16224 successfully submitted.
Receipt: # 16224-1
----- Attempting Submission 2 (Fri Jun 05 16:09:05 GMT 2020) -----
----- Attempting Submission 3 (Tue May 25 08:52:42 GMT 2021) -----
HST Phase II Proposal 16224 successfully submitted.
Receipt: # 16224-3
----- Attempting Submission 4 (Wed Jan 19 09:51:15 GMT 2022) -----
Pathways to compact white dwarf binaries
Close binaries containing at least one white dwarf (WD) are thought to be the progenitors of some of the Galaxy's most exotic objects, such as cataclysmic variables, AM CVn binaries, hot subdwarf stars, double degenerates and thermonuclear supernovae (SN), including the cosmologically important SN Ia. This zoo of possible evolutionary outcomes demonstrates the complexity of trying to study the population of WD binaries as a whole. However, without a detailed understanding of the evolution of WD binaries, we will remain unable to unravel the pathways towards thermonuclear SN and the conditions under which they ignite, and equally, we will not be able to accurately predict or model the low-frequency gravitational background from galactic WD binaries. Here we propose to take a step back in time to the last stage at which all of these systems were part of the same population of detached WD plus main-sequence star binaries. The properties of these binaries can reveal their past evolution and measure how common different evolutionary channels are. However, at optical wavelengths the WD components are overwhelmed by their main-sequence companions making it difficult to determine their masses. Using TESS data we are able to circumvent this by measuring the rotation rate of the stars and comparing this to rotational broadening measurements, to measure the binary inclinations and thus WD masses for dozens of systems. However, this method relies on the alignment of the spin and orbit of the stars which is by no means proven. Here we request HST/STIS data to confirm if our method yields the correct WD masses for these powerful probes of WD binary evolution.
The targets of this program are close (spatially unresolved by HST) white dwarf + F/G/K binaries. The main-sequence star totally dominates the optical light of these systems, and the white dwarf is the only detectable in the far-ultraviolet. We will acquire the systems on the bright main-sequence star using the standard procedure, and then switch to G140L spectroscopy of the white dwarf.
Target acquisition:
All target acquisitions require very short exposure times less, than the minimum exposure time of the STIS CCD. We have therefore set the acquisition times to that minumum value of 0.1sec. All targets are safe from saturating the acquisition exposure by a factor ~10 in exposure time.
FUV spectroscopy:
We used DA white dwarf models, which we scaled (assuming log g=8) to the Gaia parallax and GALEX FUV magnitude to estimate an effective temperature. Those scaled models were then used as input for the ETC simulator to compute the BUFFER-TIME, and gauge the expected S/N.
2 gyro mode: we do not foresee any effect on this program.
Our team possesses the knowledge and expertise to achieve the results outlined in our case. In particular, we highlight the case presented in Parsons et al. 2015, MNRAS, 452, 1754 of the supersoft x-ray source progenitor, where we established both the observational and theoretical expertise to analyse these kinds of binaries and accurately track their evolution. Our team includes:
Prof. Gansicke and Dr. Toloza are both experts in the reduction and analysis of HST COS and STIS spectroscopic data. They have extensive experience fitting the far-UV spectra of white dwarfs. They will be responsible for reducing and fitting the data to determine the white dwarf masses and temperatures of all our targets
Dr. Parsons, Dr. Raddi, Dr. Rebassa-Mansergas, Dr. Ren and Ms Hernandez are all experts in the observation and analysis of white dwarf binary systems. They have been leading the ground-based observations of these targets. They will be responsible for combining the HST and ground-based results to fully characterise each system (i.e. orbital periods, masses, temperatures, etc.) and check for consistency between the rotational broadening derived and directly measured parameters
Prof. Schreiber and Dr. Zorotovic are leading experts in binary evolution and are experienced users (and contributors) to the codes BSE and MESA. They will be responsible for simulating the past and future evolution of all our binaries
All members of our team are experienced Hubble users
Stellar Physics and Stellar Types
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