0 Assigned ID: 2946 ----- Attempting Submission 1 (Thu Mar 24 05:11:05 GMT 2022) ----- HST Phase I Proposal 2946 successfully submitted. Receipt: # 2946-1 ----- Attempting Submission 2 (Fri Mar 25 04:35:56 GMT 2022) ----- HST Phase I Proposal 2946 successfully submitted. Receipt: # 2946-2 For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave. See the COS Instrument Handbook for exceptions that may apply to observations with G130M/1291 or G160M. 0 ----- Attempting Submission 1 (Fri Jul 01 01:10:35 GMT 2022) ----- The warning regarding using all four FP-POS positions does not apply since we are using G130M/1291 which only has FP-POS 3 & 4 available. We do use both FP-POS 3 & 4. Unprecedented Light Element Abundances: Planetary Crusts or Icy Moons? The recent first-ever detections of the light elements, lithium and beryllium, in planetary bodies accreted by 'polluted' white dwarf stars, has prompted varied explanations regarding their origin. A remarkable aspect of the observations is that the abundance ratios of Li and Be relative to major elements are significantly overabundant -- for Be the overabundance is two orders of magnitude. On the one hand, these elements are dosimeters for radiation environments and may be giving us a measure of the degree of spallation production that has occurred while the exoplanetary bodies were forming. On the other hand, chemical processes such as igneous differentiation (i.e. crust formation) could be responsible. The last member of the set of light elements, boron, has never yet been observed in white dwarfs. We propose to conduct observations of the most promising WD that would be expected to display boron, and we can use the relative abundances of B and Be to discern between the possible formation scenarios. Furthermore, the proposed observations are expected to easily measure the volatiles, C and N, in our target stars, and provide important constraints on the planetary formation scenarios being tested. Only HST/COS can provide the required UV spectroscopy to observe B, C, and N, which are critical for this science. The target is a single white dwarf, and is sufficiently faint that COS safety is not a problem. Key absorption lines for our study are: B II 1362.46 Ang, C II 1334.53/1335.71 A, and N I 1243.18/1243.31 A. Our model calculations also suggest that we are likely to detect additional important elements through transitions at Al II 1191.81, P II 1154.00/1249.83A, S I 1425.03A, S II 1253.81A, and Ni II 1317.22A. Thus we use the COS G130M grating and 1291 central wavelength setting, with both segments B and A active, providing coverage of 1137-1274 A and 1292-1432 A, respectively. In this mode only two FP-POS (3 & 4) are available, which we employ to reduce fixed pattern noise. Our criterion for a spectrum that can clearly distinguish between the proposed models, is a SNR of 20 near the B II 1362 A line. From the COS ETC and our model spectrum calibrated to the GALEX FUV measured flux, this goal is achieved in four orbits. To facilitate scheduling, we split our observations into two separate visits of two orbits each. Dr. Beth Klein, and Dr. Carl Melis have extensive experience in the acquisition, data reduction and analysis of COS data (similar to what is requested in this proposal). Prof. Ben Zuckerman has led many pioneering observational studies of polluted white dwarfs. Dr. Patrick Dufour is an expert in white dwarf atmosphere models, which will be applied to derive element abundances and accretion rates from the proposed observations. Prof. Ed Young and Dr. Alexandra Doyle are cosmochemists and will contribute to the interpretation of the observed abundances. Dr. Alycia Weinberger is an expert in exoplanetary systems and spectroscopy. The PI and most Co-I's all have over a decade of experience in the study of white dwarf atmospheres, especially through high-resolution optical and/or UV spectroscopy, with half a dozen published papers on data analysis carried out with HST/COS observations and dozens of papers on white dwarfs in general. Exoplanets and Exoplanet Formation 6 false false true false false false false SUPPORTED STAR DB NO GALEX2667197548689621056 J2000 J2000 FUV=16.83 COS/FUV Spectroscopic No No G130M 1291 /Users/dr_theopolis/Documents/Proposals/HST_cycle_30/Boron/OP-cache/boron_phaseII-GO-v01.xml The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 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