0 Assigned ID: 1135 ----- Attempting Submission 1 (Fri Sep 27 15:24:18 GMT 2019) ----- ----- Attempting Submission 2 (Mon Sep 30 19:50:30 GMT 2019) ----- Hi Amber, I just added one sentence regarding the possibility of HST dropping to two gyros (=none as far as I can tell). Cheers, Boris 1581321629 ----- Attempting Submission 1 (Fri Nov 01 15:47:03 GMT 2019) ----- HST Phase II Proposal 16034 (16034.apt) successfully submitted. Receipt: # 16034-1 ----- Attempting Submission 2 (Mon Nov 04 15:47:56 GMT 2019) ----- Dissecting the evaporating atmosphere of a giant planet in a close orbit around a white dwarf with COS ultraviolet spectroscopy We have identified the first white dwarf that is photo-evaporating a close-in giant planet. The atmospheric material lost by the planet is detected via H, O, and S emission lines from a gaseous circumstellar disk, and we detect O and S in the white dwarf photosphere, indicating ongoing accretion from this disk. The accretion rate onto the white dwarf is ~3.3e9g/s, comparable to the mass loss rates of warm Neptunes. With a sub-solar upper limit of log(C/O)<-0.8, this planet may resemble warm low-metallicity Neptunes, such as HAT-P-26b. The discovery of this system opens up the unprecedented opportunity to determine the atmospheric composition of a highly irradiated gas giant via spectroscopy of the material accreted by the white dwarf, and compare the resulting abundances with planetary atmosphere models. Optical spectroscopy is limited by the lack of strong metal transitions, and hence HST's access to the far-ultraviolet is critically important for this study. We therefore propose deep COS spectroscopy to measure the abundances, or derive upper limits, of C, N, Al, Si, P, Cl, Ti, V, Cr, Mn, Fe and Ni. These elements span the majority of atmospheric species and cloud condensates that may be present in the atmosphere of the planet. This program should not be affected should HST move to a 2-gyro mode. The goal of these observations is to obtain a high signal-to-noise far-ultraviolet spectrum of the white dwarf WDJ0914+1914, which hosts, and evaporates a close-in giant planet. Some of the atmospheric material accretes onto the white dwarf, and the planned COS spectroscopy will be used to measure the abundances of that material from the sharp photospheric metal lines. We use the G130M grating with two central wavelengths to maximise the wavelength covered by these observations, and to achieve gap-less coverage. We make use of all permitted FP-POS positions, i.e. 3 & 4 for @1291A, and 1,2,3,4 @ 1222A. The expected period of the planet is ~15 days, and there is a chance that part of the evaporating atmosphere crosses our line-of-sight onto the white dwarf, which would result in the transient appearence of resonance absorption lines of O, S, C, or N. We therefore plan the observations as ten individual orbits with a separation of 1.3-1.7 days between them. Gaensicke has been PI of 20 HST programs, carrying out far-ultraviolet spectroscopy of white dwarfs, including large, medium, small GO programs and several snapshot programs. He has in-depth experience in the analysis and interpretation of the observations of accreting white dwarfs, both in binary systems, and evolved planetary systems. He will implement the observations, and lead the analysis. Schreiber is a theoretical astrophysicist with key interests in accretion discs, the evolution of binary stars, and proto-planetary disks. He is leading the development of the irradiation model for WDJ0914. Toloza is an expert in the analysis of COS time-tag observations. She will carry out the data reduction and the computation of white dwarf model atmospheres using the code of Detlev Koester. Gentile-Fusillo identified WDJ0914+1914 as a peculiar white dwarf, and he will contribute to the write-up of the results. Koester has developed the model atmosphere code that will be used for this project, and he will provide guidance on the use of the code. Manser is an expert on gaseous debris disks at white dwarfs, and he will contribute to the discussion of the line morphology. Planets and Planet Formation 3 false false true false false false false SUPPORTED STAR DA NO J2000 J2000 GALEX FUV=17.77 +- 0.06 The scheduling data was generated by CASM 27.2. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G130M 1222 The scheduling data was generated by CASM 27.2. CASM was run in Phase I mode. COS/FUV Spectroscopic No No G130M 1291 /tmp/OPVisit1826479474647441597.xml Timing link suitability includes constraints ([02 After 01 by 1.3 to 1.7 days]) The scheduling data was generated by CASM 27.2. CASM was run in Phase II mode. 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