0Assigned ID: 1072
----- Attempting Submission 1 (Tue Feb 26 00:57:26 GMT 2013) -----
HST Phase I Proposal 1072 (DBZ.apt) successfully submitted.
----- Attempting Submission 2 (Thu Feb 28 05:04:57 GMT 2013) -----
HST Phase I Proposal 1072 (DBZ.apt) successfully submitted.
----- Attempting Submission 3 (Thu Feb 28 19:57:36 GMT 2013) -----
HST Phase I Proposal 1072 (DBZ.apt) successfully submitted.
----- Attempting Submission 4 (Fri Mar 01 18:33:50 GMT 2013) -----
HST Phase I Proposal 1072 (DBZ.apt) successfully submitted.
----- Attempting Submission 5 (Fri Mar 01 18:42:52 GMT 2013) -----0----- Attempting Submission 1 (Sat Jun 15 00:44:21 GMT 2013) -----
----- Attempting Submission 2 (Wed Jan 29 23:39:00 GMT 2014) -----
----- Attempting Submission 3 (Thu Jan 30 03:04:02 GMT 2014) -----The Elemental Compositions of Extrasolar Minor PlanetsWe propose to observe five white dwarfs known to be polluted by accretion of their own asteroids in order to investigate three related questions. (1) What determines carbon abundances within extrasolar asteroids? (2) Can we identify water-rich extrasolar planetesimals? (3) Can we find evidence for silicon-rich planetesimals, as would be expected if they are largely composed of crustal material? Data from these 5 proposed targets combined with previous COS observations either by ourselves or others of 6 additional targets, will complete an ultraviolet spectroscopic mini-survey of all known highly polluted white dwarfs with helium-dominated atmospheres within 80 pc of the Sun. This study will provide a unique legacy for understanding the formation and evolution of extrasolar rocky planets.Extrapolating from our ground-based observations of Ca II 3933 A and Mg II 4481 A and scaling from optical and ultraviolet data for GD 40 and G241-6 (Klein et al. 2010, 2011, Jura et al. 2012), we expect some photospheric lines such as Si II 1265 A and O I 1152 A to be stronger than 50 mA and therefore detectable in all of our targets. If C has nearly a "solar" abundance, we also will detect photospheric C II 1336 A; the detection of Fe is uncertain. With these data, we will be able to investigate all three science questions.
Paralleling the strategy described in Jura et al. (2012), we propose to obtain spectra with the G130M grating in the FUV module with a central wavelength of 1291 A. For allfive targets, we estimate the flux at 1350 A, near the wavelengths of the important C II lines, from measured GALEX FUV-band (1530 A) magnitudes and our COS spectra and/or models of stars of similar temperature such as GD 40. We then use the COS ETC 21.1 to determine the required on-target observing time to achieve a signal-to-noise ratio (SNR) of 30 in all targets except HS 2253+8023 where we propose to achieve a SNR of 20. We include the overheads for target acquisition and instrumental set-up to determine the requested number of orbits. Our targets are sufficiently faint that COS safety is not a problem.Position and proper motion is from PPMXL catalog (2010).EXTRA-SOLAR PLANETSDefaultfalsefalsefalsefalsefalseSUPPORTEDSTARDBEXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMJ2000J2000STARDBEXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMSDSSJ101437.09+564832.6J2000J2000STARDBEXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMSDSSJ142736.05+534828.4J2000J2000STARDBEXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMSDSSJ171155.66+230101.1J2000J2000STARDBEXTRA-SOLAR PLANETEXTRA-SOLAR PLANETARY SYSTEMJ2000J2000COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291The scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.138716443800090.16685725490692(Tic-Visit
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