0Assigned ID: 4031
----- Attempting Submission 1 (Mon May 22 16:50:11 GMT 2023) -----
HST Phase I Proposal 4031 successfully submitted.
Receipt: # 4031-1
----- Attempting Submission 2 (Wed May 24 11:57:23 GMT 2023) -----
HST Phase I Proposal 4031 successfully submitted.
Receipt: # 4031-2
----- Attempting Submission 3 (Wed May 24 11:59:50 GMT 2023) -----
HST Phase I Proposal 4031 successfully submitted.
Receipt: # 4031-3
----- Attempting Submission 4 (Wed May 24 14:31:47 GMT 2023) -----ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
INEFFICIENT ORDERING OF FP-POS POSITIONSOne of the orbits in visit 3 failed, so I added a 5th visit (1 orbit) to repeat the observation (approved in HOPR 93077).-1405779296----- Attempting Submission 1 (Fri Sep 08 16:53:23 GMT 2023) -----
----- Attempting Submission 2 (Thu Nov 30 19:17:10 GMT 2023) -----
----- Attempting Submission 3 (Sat Jan 18 15:12:30 GMT 2025) -----There is a warning about my not using all 4 FP-POS positions, but I think this is acceptable since the other two positions were used in the first orbit of visit 3.
There are also some "orbit visibility overrun" warnings about visits 1 and 4, but those have already been completed, so I think they can be ignored.UV spectroscopy of runaways from thermonuclear supernovaeWe propose COS FUV spectroscopy of four newly-discovered hypervelocity white dwarfs that are runaways from double white dwarf binaries in which one component exploded in a type Ia supernova. Our targets have radial velocities ranging from 1100 to 2300 km/s -- the fastest stellar radial velocities ever measured. They are hot (20,000-140,000 K) and bright in the UV. The primary goal is measurement of their abundance patterns, particularly the abundances of Fe, Si, Mg, and Mn. The surfaces of these stars are predicted to be heavily polluted with supernova ejecta. Abundance measurements will constrain the yields of the supernovae from which these stars were born and the masses of the exploded white dwarfs, both clarifying their formation histories and informing models for their thermal evolution. Optical spectroscopy has shown that their atmospheres consist mostly of carbon and oxygen, but the abundances of most metals can only be measured in the UV at these temperatures.We will obtain 11 orbits of HST/COS medium-resolution FUV spectroscopy of four hot, inflated WDs. The three brightest objects, with FUV = 17.9, 18.0, and 18.2 mag, will be observed for two orbits each, while the faintest target, with FUV = 19.5 mag, will be observed for 5 orbits. The FUV magnitudes are measured from GALEX for two targets and estimated based on the effective temperature and optical SED for the other two. The extinction is low ($E(B-V) < 0.2$), and the expected FUV magnitudes are well-constrained. None of the targets have nearby bright UV sources that would risk damaging the detector.
We will acquire each target using the NUV channel with an ACQ/IMAG sequence, and then switch to the FUV channel, using the G140L grating with the 1105 AA central wavelength, spanning 1130-2000 AA. Detailed modeling of the photospheric abundances (particularly Fe, Si, Mg, and Mn), requires a signal-to-noise ratio ~30. Using the COS ETC with model spectra generated for our targets based on their optical spectra and broadband SEDs, and accounting for the targets' individual visibility windows and instrumental overheads, we find that we can achieve SNR = 26-33 at 1300 AA in one orbit each for the 3 brightest targets, and SNR = 20 in 5 orbits for the faintest target.PI El-Badry discovered these objects. He is experienced in optical and UV spectroscopy and will lead the planning and analysis of the observations. CO-I Shen is an expert in modeling double-degenerate mergers; he pioneered the D6 scenio and will aid in theoretical interpretation of the results. CO-I Gaensicke is an expert in optical and UV observations of white dwarfs and an experienced user of HST/COS. He will aid in planning the observations and interpretting the results.Stellar Physics and Stellar Types6falsetruefalsefalsefalsefalseSUPPORTEDSTARSDONOJ2000J2000NUV = 18.89, FUV = 19.49STARSDONOJ2000J2000NUV = 18.3, FUV = 18.0STARSDONOJ2000J2000NUV = 18.4, FUV = 18.2STARSDONOJ2000J2000NUV = 18.23, FUV = 17.94COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode./private/var/folders/_4/hh3dgzmd13l0wvjyf6tkz1cm0000gn/T/OPVisit2505470892036431863.xml171263756800061.97246783348811(Tic-Visit
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