0Assigned ID: 888
----- Attempting Submission 1 (Fri Apr 05 22:48:23 GMT 2019) -----The number of orbits used exceeds the number allocatedrepeat of 6 orbits due to failute in guiding star (3 of 6,576
HOPR 92082)1778089499----- Attempting Submission 1 (Thu Jul 04 15:15:54 GMT 2019) -----
----- Attempting Submission 2 (Wed Aug 07 16:34:19 GMT 2019) -----
----- Attempting Submission 3 (Thu Jun 17 16:58:07 GMT 2021) -----
----- Attempting Submission 4 (Fri Jun 25 15:34:59 GMT 2021) -----
----- Attempting Submission 5 (Tue Aug 31 20:33:40 GMT 2021) -----APT complains about the inefficient use of FP-POS movements - that's not an issue for us as we move during Earth occultationMapping the distribution of the planetary debris accreted across the surface of the white dwarf G29-38Measuring the bulk composition of exo-planets is crucial for the development of planet formation theories, and currently the only available method is spectroscopy of white dwarfs accreting planetary debris. The photospheric abundances of these white dwarfs reflect the bulk compositions of the accreted parent bodies, entirely analogous to meteorite abundance studies. HST ultraviolet spectroscopy has played a pivotal role in this field, providing abundance measurements of many elements inaccessible from the ground. The bulk compositions measured so far are broadly similar to those found in the solar system, suggesting that planet formation may be a fairly uniform process. The accuracy of the measured bulk compositions relies on the physically correct analysis of the white dwarf spectroscopy. However, all studies have so far used an assumption that remains untested - that the metals are uniformly distributed over the stellar surface. Given accretion proceeds via a geometrically thin disk, the validity of this assumption is far from obvious. We propose deep COS time-series ultraviolet spectroscopy of G29-38, the prototype white dwarf accreting from a debris disk. G29-28 undergoes non-radial pulsations, which heat localized regions on its surface that can briefly dominate the flux of the star. A spectrum obtained during such a heating event reflects the abundances of a small patch on the white dwarf surface. We will analyze a sufficiently large number of pulses to accurately map the distribution of metals across the entire surface of G29-38. Our results will be used to improve the modelling of debris-accreting white dwarfs, and lead to more reliable bulk compositions.The goal of this program is to obtain time-tagged UV spectroscopy of the pulsating white dwarf G29-38 simultaneous to the Sector 16 TESS observations (2019, Sept 11 - Oct 7). The pulsations have periods in the range of two to 20 minutes. For the time-domain analysis, we require to pack the HST observations in the longest possibe contiguous COS visits, as irregular gaps in between multiple short visits will create a window function that is difficult to deal with. In an ideal world, the observations should be done in a single 35-orbit visit - which may not be feasible.
In this first attempt, we opt for 5 x 7-orbit visits. Grouping the observations in fewer but longer visits would be helpful.
We simulated both imaging and target acquisitions using a white dwarf model spectrum with the appropriate average temperature and surface gravity, scaled to the Gaia distance to the target, and find that the imaging acquisition using MIRROR-A and BOA is the fastest option. These average atmospheric parameters were measured from the previous COS/G130M observation of G29-38 (four orbits, data sets LBHK55010 and LBHK05010 ).
We use the 1291A central wavelength because it provides the optimum wavelength coverage, including the broad quasi-molecular features at ~1150A and ~1400A, which is very temperature-sensitive, the Si II lines at 1260,65, the CII lines at 1335, and the OI line at 1152A. Because the star is undergoing pulsations, we use the TIME-TAG mode and switch between FP-POS 3 and 4, and we will re-construct spectra phased on the pulsation modes.
APT warns about inefficient FP-POS movements (4->3) - as we do those during Earth occultation, it does not affect the performance of the program.
2019-Aug-07: following the request of Juila we switched from an imaging acquisition to a spectroscopic acquisition as there is an M-dwarf near our target, and there is the risk it could end up in the second aperture during an imaging acquisition.
2021-Jun-17: the 90 sec overrun in the exposures was removed. And resubmitted. In addition the BETWEEN was modified to 2021-Aug-20 to 2021-Sept-16
2021-Jun-25: The exposure of each orbit was reduced by 45 sec to accomodate the visibility, as requested.Toloza has initiated this project as part of her PhD, and has detailed experience in the analysis of COS observations, white dwarf atmosphere models, and in observations and the interpretation of accreting binaries. She has used the archival HST observations to demonstrate the feasibility of the proposed observations.
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.
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.
Montogmery is an expert on white dwarf asteroseismology, and has carried out several studies of G29-38. He will lead the asteroseimological analysis of the TESS light curve, identify pulsation modes, and compute the geometry of the pulsations during the epochs of the HST observations.
Hambsch, Monard, Boyd and Vanmunster will obtain additional time-series photometry of G29-38 using different filters on each observing site, and hence provide colour information which will complement the TESS data.Planets and Planet FormationStellar Physics0falsefalsetruefalsetruefalsefalsefalseSUPPORTEDSTARDANOThis target was observed with COS/G130M as part of HST program 12290, data set LBHK55010.J2000J2000COS/FUVSpectroscopicNoNoG130M1300The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.1630315939000223.3906436458724(Tic-Visit
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:proposal-id 15839
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)
(Tic-Orbit
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)false70