0 Assigned ID: 337 ----- Attempting Submission 1 (Fri Apr 08 01:00:57 GMT 2016) ----- For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting. For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting. Just a heads-up: This is my first Phase II submission, but I was assisted by Boris Gaensicke, who has submitted many Phase II HST/COS proposals. Please let me know if we should relax any orbit visit constraints to ensure feasibility. Thank you! 863594338 ----- Attempting Submission 1 (Mon Jul 11 11:21:33 GMT 2016) ----- Submission failed due to error communicating with the submission server. Please retry in a few minutes. If this error persists please contact the help desk at help@stsci.edu ----- Attempting Submission 2 (Mon Jul 11 11:22:40 GMT 2016) ----- To most optimize our two three-orbit visits and minimize any lost time we suggest using only three FP-POS positions rather than four. Most stars in our Galaxy will end or have already ended their lives as white dwarf stars, making them important benchmarks for stellar evolution. Here we propose to obtain COS far-ultraviolet spectroscopy of a pulsating hydrogen-atmosphere white dwarf (DAV) with extensive, space-based photometry obtained by the Kepler spacecraft during the K2 mission. The pulsation spectrum is the richest of any DAV collected to date, but to extract any information about the white dwarf interior we must identify the spherical degree (l) of the modes present. Our time-tagged ultraviolet observations will enable us to identify the spherical degree of the highest-amplitude pulsation modes, since the ratios of the ultraviolet-to-optical pulsation amplitudes strongly depend on the geometry of the pulsation modes. This will decisively determine if most of the modes present are a series of l=3 modes, as it appears from the frequency multiplets in the K2 data; however, l=3 modes have never been clearly identified in a pulsating white dwarf. Our far-ultraviolet spectroscopy, covering the H2/H2+ quasi-molecular satellites around 1400 and 1600 AA, will also measure the white dwarf temperature and mass to an accuracy unachievable from the ground. This robust temperature and mass will anchor our detailed asteroseismic investigation of this stellar remnant. The unique combination of HST and Kepler observations will make this white dwarf a benchmark for the unprecedented opportunities for white dwarf archaeology enabled by the original Kepler mission and its extension into the ecliptic, K2. The two main goals of our observations are to measure the atmospheric parameters of this pulsating white dwarf and to measure the far-UV pulsation amplitudes. Using the COS G140L grating centered at 1105 AA, we cover the appropriate spectral features at sufficient spectral resolution to accurately determine the atmospheric parameters. The time-series photometry from the time-tagged data will require slightly more planning. In summary, we request our two three-orbit visits to be separated by 2.2 days (up to no more than 6.0 days separating the visits) in order to fully resolve the pulsations, which in the nearest case are separated by as little as 5.5 microHz. Further information and justification is found in the Description of the Observations section of the accepted proposal. Stellar Physics 12 false true false false false false SUPPORTED STAR ZZ CETI STAR NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 g=17.12 COS/FUV Spectroscopic No No G140L 1105 COS/FUV Spectroscopic No No G140L 1105 1468235223883 /private/var/folders/3j/vrqz5rxs4dn33vngrdfw39x00000gn/T/OPVisit6477692628488909342.xml Timing link suitability includes constraints ([02 After 01 by 2.2 to 6.0 days]) The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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