0Assigned ID: 1233
----- Attempting Submission 1 (Sat Jan 18 00:31:08 GMT 2020) -----
HST Phase I Proposal 1233 (newdiscs.apt) successfully submitted.
Receipt: # 1233-1
----- Attempting Submission 2 (Sat Jan 18 00:38:46 GMT 2020) -----
HST Phase I Proposal 1233 (newdiscs.apt) successfully submitted.
Receipt: # 1233-2
----- Attempting Submission 3 (Sat Jan 18 02:21:46 GMT 2020) -----0----- Attempting Submission 1 (Tue Mar 17 17:51:51 GMT 2020) -----
----- Attempting Submission 2 (Mon Apr 06 16:10:18 GMT 2020) -----Exploring evolved planetary systems: three new debris discsHSTIt is now established that planets survive the evolution of their host star into a white dwarf. Planetary remnants around a number of these ancient stars are revealed by compact debris disks, formed from the tidal disruption of planetesimals, which are detectable as IR flux excess. Accretion from these disks results in metal pollution of the otherwise pristine H or He white dwarf atmospheres, and the analysis of adequate optical and UV spectroscopy of these systems allows to reconstruct the bulk composition of the disrupted planetesimals.
Quantitative insight into the structure, formation and evolution of the parent bodies arises from mineralogical studies of the dusty disks, but requires sensitive IR spectroscopy which is currently available only for one single system. Even though the imminent launch of JWST will greatly improve the IR spectroscopic capabilities, the analysis will remain subject to degeneracies due to the relatively flat and broad features of different dust components. However, with the elemental abundances of the dust in hand, established from HST/COS observations of the same systems, these degeneracies can be broken, and will dramatically augment our knowledge of the composition and structure of rocky exo-planets.
We have identified three new debris disks, and request here a modest amount of COS mid-cycle spectroscopy to fully characterise the elemental abundances of the dust in time for JWST Cycle 2 proposals. Cycle 28 observations will, at best, leave little time for the required analysis, but more likely slip beyond the JWST Cycle 2 deadline.The goal of these observations is to obtain high signal-to-noise far-ultraviolet spectra of three white dwarfs which are accreting planetary debris from circumstellar debris disks. 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 @1291A and @1222A observations are split into two separate visits to facilitate the scheduling.
This program should not be affected in case that HST moves to a 2-gyro mode.Gentile Fusillo has been using large astronomical surveys to (a) identify white dwarfs, most recently producing the first all-sky catalogue of white dwarfs using Gaia DR2, and (b) to then search for white dwarfs with signature of evolved planetary systems. He identified two of the targets of this proposal.
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.
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.
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.
Manser is an expert on gaseous debris disks at white dwarfs, and he will contribute to the discussion of the line morphology. He recently identified the first spectroscopic signature of a solid planetesimal.
Dennihy and Manser are working on models for the assymetric Ca II emission lines in WDJ0347+1624.Planets and Planet Formation0falsefalsetruefalsetruefalsefalseSUPPORTEDSTARDANOJ2000J2000GALEX FUV=16.0415 GALEX NUV=16.4401STARDANOJ2000J2000GALEX FUV=16.9069 GALEX NUV=17.2377STARDANOJ2000J2000GALEX FUV=15.8816 GALEX NUV=16.1392COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG130M1291The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./tmp/OPVisit16322388260949458582.xmlOnly two FP-POS settings allowed for the 1291A central wavelength.(Tic-Visit
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