0 Assigned ID: 562 ----- Attempting Submission 1 (Fri Apr 07 15:17:04 GMT 2017) ----- For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details. Dear John & Amber, here is the resubmission after switching the planned near-UV spectroscopy from COS to STIS, as approved via the TTRB request. Balancing all goals, we decided to drop one target and increase the S/N in the remaining two. Boris 705993141 ----- Attempting Submission 1 (Thu Jul 20 23:57:08 GMT 2017) ----- ----- Attempting Submission 2 (Fri Aug 11 13:10:29 GMT 2017) ----- APT warns about not using all FP-POS settings, but that's per COS 2025 procedures. A Detailed Study of Rocky Planetary Material in the Hyades The Hyades is the nearest open cluster, relatively young, and containing numerous A-type stars. Its youth, distance, and metallicity make it an ideal site to study planet formation around 2-3 Msun stars, and in a dynamically challenging environment. During our HST COS Snapshot, we discovered the ongoing accretion of Si-rich and C-deficient material in two white dwarf Hyads. The lower limit Si/C ratios determined from these 400s exposures indicate the material is more C-depleted than in chondritic meteorites, the most primitive rocks in the Solar System. Our 2013 Keck discovery of metal pollution in a third Hyades white dwarf indicates that planet formation is common in the cluster. Together, these three stars indicate that substantial minor bodies persist at several AU or more, and provide an unprecedented opportunity for a detailed study of rocky exoplanet precursors in a cluster environment. We propose to obtain detailed abundances of the planetary debris at these three polluted Hyads, which requires a modest investment of observatory time. The mass ratios between C, O, Mg, and Si are accurate indicators of the temperature and orbital regions where the parent bodies formed, their water and volatile contents. We will also detect Al and Fe, which are key indicators of differentiation and giant impacts among planetary embryos. Our proposed observations will provide legacy value for planet formation models, and especially those in cluster enviroments. These observations cannot be done from the ground or at optical or longer wavelengths, and must be carried out by HST in the ultraviolet. In previous G130M COS observations, we detected photospheric metal contamination in these two Hyades white dwarfs, demonstrating that they accrete planetary debris. Here, we will obtain much deeper ultraviolet spectra spanning a wider wavelength range, probing for additional elements (C, Fe, Al, O, Mg). * WD0421+162: we obtained a short (400sec) COS G130M@1291A spectrum as part of our snapshot survey. Critical lines are at 1152A, 1260/65A, ~1290-1340A, ~1390-1403A. Because of the COS 2025 strategy, we will not be able to execute the observions @ 1291A with all FP-POS settings. To mitigate this, we will use one orbit @1291A, using FP-POS 3/4, and one orbit @1222A, using FP-POS 3/4, combining those two settings will provide particularly good coverage of the O I 1152A line. In addition, we will obtain COS G160M spectroscopy (Al 1670A) and STIS G230M (Mg 2800A). * WD0437+138: we obtained good G130M spectra as part of program 14597, here we will obtain COS G160M and STIS G230M spectroscopy. Planets and Planet Formation Stellar Physics 6 false true false false false false SUPPORTED STAR DA NO White dwarf in the Hyades, d=47pc, Teff=19322K, logg=8.10. Observed with COS/G130M: LBIYA8010 J2000 J2000 GALEX FUV=13.75836 GALEX NUV=13.89075 STAR DA NO White dwarf in the Hyades, d=45pc, Teff=15120K, logg=8.25 Observed with COS/G130M: LDAO08010 J2000 J2000 GALEX FUV=15.43189 GALEX NUV=14.84796 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G160M 1611 COS/FUV Spectroscopic No No G160M 1611 COS/FUV Spectroscopic No No G160M 1611 COS/NUV Spectroscopic No No G285M 2676 COS/NUV Spectroscopic No No G285M 2676 The scheduling data was generated by CASM 25.2. 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