0 Assigned ID: 2813 ----- Attempting Submission 1 (Mon Mar 21 20:18:53 GMT 2022) ----- ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS 0 ----- Attempting Submission 1 (Sat Jun 25 20:54:03 GMT 2022) ----- ----- Attempting Submission 2 (Tue Apr 23 04:10:04 GMT 2024) ----- FP-POS ordering is not inefficient, it is increasing within each orbit. Visit 51 has already executed. Are all massive Kuiper belt objects built the same? We have identified GaiaJ0628-5054 as a single, polluted, white dwarf star that is accreting extremely oxygen- and hydrogen-rich material that is otherwise depleted in all other rocky elements, suggesting that it is being polluted by a massive icy body. Similarities with the hitherto unique extrasolar Kuiper belt object-ingesting WD1425+540 suggest GaiaJ0628-5054 is being polluted by what could be a rare second example of an extrasolar Kuiper belt object. We propose COS FUV spectroscopic observations of GaiaJ0628-5054 that will allow us to confirm our interpretation and then explore the range of rocky mass fractions for extrasolar Kuiper belt object analogs. These observations will have immediate value in assessing the validity of internal structure models for Pluto, Charon, and Arrokoth by providing a contrast of New Horizons interpretations for outer solar system bodies against what is observed in other planetary systems. Our primary goal is to further assess the O-rich and rocky element-poor (Si, Fe) nature of the polluted white dwarf star GaiaJ0628-5054 and determine how much C, N, and S are present to identify the origin of the accreted parent body. Our secondary goal is then to characterize additional elements that may enhance our understanding of the accreted material which appears to be a Kuiper belt object analog. Modeling of absorption lines shows that the desired elements can be measured or sufficiently strongly constrained with observations in the 1100-1350 Angstrom range. We will perform medium spectral resolution ultraviolet spectroscopy with COS and the G130M grating to cover the 1100-1350 Angstrom range. No GALEX-measured FUV flux exists for GaiaJ0628-5054; we instead estimate an FUV AB magnitude of 17.0 based off of spectral energy distribution fitting to optical and infrared data combined with an accurate atmospheric model that fits them. We estimate how much time on source is necessary to obtain our desired signal-to-noise with this estimated FUV magnitude and a small amount of interstellar reddening (consistent with its location in the Galaxy). It should be possible to obtain average signal-to-noise~20 in the 1100-1350 Angstrom wavelength range with total on-source exposure time of roughly 12,000 seconds. These estimates are made using the COS ETC assuming standard background parameters and with a white dwarf spectral energy distribution matched to the parameters and flux level of our target. Our requested time estimates for COS are increased assuming 20 minutes of instrument overhead (including all acquisition and exposure overheads as suggested in the COS manual) per visit and 6 minutes of observatory overhead per orbit (spacecraft acquisition). In sum, we request 5 orbits total for COS observations of Gaia J0628-5054. Observations will be done in the TIME-TAG mode using TAG-FLASH wavelength calibration. The target white dwarf is an ICRS object (Gaia DR3 position with less than 0.4" positional uncertainty), has an estmated UV flux, and is safe for the COS detectors in our desired setups. The proposal team has extensive experience with obtaining, reducing, and analyzing COS data. We have been working closely as a team to produce such results since 2011 and are world experts in investigating the mineralogy of white dwarf atmospheric pollutants (the main scientific goal of the proposed project). Dr. Carl Melis has led several separate COS polluted white dwarf projects, one of which has been published (Melis & Dufour 2017, ApJ 834, 1), and others are in preparation to be submitted in 2022 as of the writing of this statement. Drs. Zuckerman, Xu, and Klein (with now-deceased Prof. Mike Jura) have been obtaining COS spectra of polluted white dwarfs for several years and have produced a similar number of publications (e.g., Jura et al. 2012, ApJ 750, 69; Xu et al. 2013, ApJL 766, 18; Xu et al. 2013, ApJ 766, 132; Xu et al. 2014, ApJ 783, 79; Xu et al. 2017, ApJL 836, 7). Dr. Weinberger is an expert in exoplanetary systems and spectroscopy. Prof. Dufour has substantial experience in modeling white dwarf spectra, especially to get atmospheric parameters and abundances, and has also led his own COS projects that have resulted in publications (e.g., Dufour et al. 2011, ApJL 733, 19). All members of the proposal team are devoting significant fractions of their time to studying polluted white dwarf stars. They will continue to do so with this project if time is awarded. Drs. Melis, Klein, Xu, and Weinberger will contribute to data reduction and analysis. Prof. Dufour will be responsible for modeling spectra and measuring abundances. All will contribute to interpretation and publication. Exoplanets and Exoplanet Formation Solar System Astronomy 6 false false true false false false false false SUPPORTED STAR DB NO Gaia DR3 Main astrometry. GAIAJ0628-5054 J2000 J2000 mFUV~17 COS/FUV Spectroscopic No No G130M 1222 The scheduling data was generated by CASM 32.0. CASM was run in Phase II mode. 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CASM was run in Phase II mode. G130M grating observations of GaiaJ0628-5054. 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CASM was run in Phase II mode. G130M grating observations of GaiaJ0628-5054. 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