final97436022Assigned ID: 29
----- Attempting Submission 1 (Wed Apr 02 13:59:12 GMT 2014) -----
HST Phase I Proposal 29 (wired_disk_22.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 03:57:36 GMT 2014) -----
HST Phase I Proposal 29 (wired_disk_22.apt) successfully submitted.
----- Attempting Submission 3 (Fri Apr 11 19:03:34 GMT 2014) -----
HST Phase I Proposal 29 (wired_disk_22.apt) successfully submitted.
----- Attempting Submission 4 (Fri Apr 11 19:05:47 GMT 2014) -----
HST Phase I Proposal 29 (wired_disk_22.apt) successfully submitted.
----- Attempting Submission 5 (Fri Apr 11 22:22:10 GMT 2014) -----
HST Phase I Proposal 29 (wired_disk_22.apt) successfully submitted.updated ACQ/IMG exposure time for Visit 2 due to mistaken NUV magnitude.-377249956----- Attempting Submission 1 (Mon Jul 21 09:58:39 GMT 2014) -----
----- Attempting Submission 2 (Thu Oct 30 19:53:12 GMT 2014) -----An autopsy of dead planetary systems with COSWe propose to use HST/COS to conduct autopsies of dead planetary systems around UV bright hydrogen-white dwarfs (WDs), which have dust disks found via their mid-IR emission in excess of that expected from the photosphere. As part of a WISE survey, and followed up with a combination of NASA Keck HIRES/Magellan MIKE optical spectroscopy, we have identified three new systems that are accreting dust. These WDs are bright in the mid-IR and UV, gold-standard targets for studies with HST/COS and later with JWST. The dusty material is debris resulting from the tidal disruption of exo-asteroids that accrete onto the WD surface. Many atomic elements from the accreted and dissociated dust particles are detectable with COS, enabling abundance determinations of exo-asteroidal material. Moreover, the photospheric abundances of this material can be directly compared with a determination of the dust mineralogy obtained with future JWST mid-IR spectroscopy-our proposed UV observations provide complementary constraints on mineralogical compositions of the accreting dust particles.
UV spectroscopy is crucial for cataloging elemental abundances for these exo-asteroids. For the majority of WDs, optical spectroscopy reveals only a couple of lines of Ca or Mg, while UV spectroscopy captures lines from Al, Fe, Si, C, Ni, O, S, Cr, P, and Ti. Obtaining the elemental abundances of exo-asteroids is comparable to the spectroscopic characterization of transiting exoplanets or protoplanetary disks-all of these techniques determine how the chemical diversity of planetary systems translate into planetary architectures and the probability of habitable planets around solar-type stars.We wish to acquire each object with an ACQ/IMAGE exposure, then followed by FP-POS=ALL observing at G130M/1291 within one orbit. Target S/N of at least 30 within an orbit.DEBRIS DISKSDefaultfalsetruefalsefalsefalseSUPPORTEDSTARDAPM from UCAC4, position from 2MASS, uncertainty on proper motion is ~0.06" from the epoch (1-sigma)J2000J2000STARDAPM from UCAC4, position from 2MASS, PM uncertainty ~0.06" from epoch.J2000J2000FUV=14.94STARDAcoordinates taken from 2MASS, proper motion from UCAC4. uncertainty in proper motion may place star up to ~0.1" away from expected position (1-sigma), still within 0.4" error budgetJ2000J2000FUV=13.93COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1291The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode./private/var/folders/9d/jk8g77fd2jx3sxdb33rhwx48000300/T/OPVisit5697450892365142142.xmlGALEX FUV=14.95, NUV=15.154--will achieve S/N=25 @ longer wavelengths
4 FP-POS after ACQ/IMAGE with MIRRORB/PSA(Tic-Visit
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4 FP-POS after ACQ/IMAGE with MIRRORA/BOA(Tic-Visit
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)true10The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode./private/var/folders/9d/jk8g77fd2jx3sxdb33rhwx48000300/T/OPVisit3950263343210670887.xmlGALEX FUV=13.93, exposure time chosen to fill standard orbit. Can be shortened to accomodate additional scheduling flexibility.
4 FP-POS after ACQ/IMAGE with MIRRORA/BOA(Tic-Visit
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