0Assigned ID: 386
----- Attempting Submission 1 (Fri Mar 06 03:45:59 GMT 2020) -----
HST Phase I Proposal 386 successfully submitted.
Receipt: # 386-1
----- Attempting Submission 2 (Fri Mar 06 20:08:23 GMT 2020) -----
HST Phase I Proposal 386 successfully submitted.
Receipt: # 386-2Please include Co-I Erik Dennihy (edennihy@gemini.edu) in any correspondence. Thanks!-1204968893----- Attempting Submission 1 (Thu Jun 25 14:34:54 GMT 2020) -----A New Method to Measure the Chemical Compositions of Extrasolar PlanetesimalsThe chemical composition of an extrasolar planet is a fundamental property with little observational signature. Spectroscopic observations of polluted white dwarfs have proven to be a successful pathway to constrain the compositions of disrupted planetesimals but this approach has its own limitations. Here, we propose a new method to measure the compositions of extrasolar planetesimals by observing the gas debris around polluted white dwarfs. These disks are fresh extrasolar planetary material in a transient stage, right after tidal disruption and before being completely accreted onto the white dwarf. Recent increases in the sample size of white dwarf gas disks combined with timely advancements in disk modeling efforts have made this new exploration feasible. This proposal will open a noval method to measure chemical compositions of extrasolar planetesimals.The goal of this proposal is to determine the magnesium abundances in gas disks around white dwarfs -- a novel way to measure the compositions of extrasolar planetesimals. The strongest magnesium transitions are those around Mg II 2800 A. We propose to use G230L grating (spectral resolution 2000) with a central wavelength of 2950 A, which covers 1651 - 2049 A and 2751 - 3150 A. Such a wide wavelength coverage will allow us to search for other unknown gas emission lines as well.
For the four systems with strong calcium triplet emissions, a SNR of at least 30 is needed to distinguish different Mg abundances, while for four systems with weaker calcium triplet emission, a SNR of at least 50 is needed. The requested time is computed with the exposure time calculator v28.1. Including overhead for target acquisition, a total of 16 orbits is needed for this program. Our targets are sufficiently faint that the safety of COS is not a concern.
The reduced gyro operations have little impact on the execution of this program.Our team is experienced in characterizing white dwarf planetary systems. Dr. Klein, Dr. Melis, Dr. Xu, and Dr. Zuckerman have extensive experience with COS observations and data analysis, and have led several studies on polluted white dwarfs observed with COS. Dr. Dennihy, Ms. Doyle, Dr. Jiang and Dr. Melis have performed ground based spectroscopic observations of hundreds of new Gaia white dwarfs and identified these 8 new gas disk systems. Dr. Yeh and Dr. Wang are expert Cloudy users and will perform gas disk modeling. Dr. Dufour produces state of the art white dwarf model atmosphere calculations that will be directly compared to the disk measurements.Exoplanets and Exoplanet FormationStellar Physics and Stellar Types6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARDANOJ2000J2000STARDANOJ2000J2000STARDANOJ2000J2000STARDANOJ2000J2000STARDANOJ2000J2000STARDANOJ2000J2000STARDBNOJ2000J2000STARDANOJ2000J2000COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.(Tic-Visit
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