0
Assigned ID: 5140
----- Attempting Submission 1 (Mon Mar 25 01:46:52 GMT 2024) -----
Updated Visit 19 and 20 to use Mirror B with PSA for ACQ.
Visit 07 failed, and time was given to repeat the visit and this is now visit 34.
Visit 09 failed, and time was given to repeat the visit and this is now visit 35.
Visit 08 had half the intended exposure, and time was given to complete the second orbit and this is now visit 36.
Visit 14 had guide star issues, and time was given to repeat the second orbit and this is now visit 37.
Visit 28 failed, and time was given to repeat 1 orbit and this is now visit 38.
-1925242945
----- Attempting Submission 1 (Tue Aug 13 16:55:27 GMT 2024) -----
----- Attempting Submission 2 (Wed Dec 11 14:28:37 GMT 2024) -----
----- Attempting Submission 3 (Fri Mar 21 20:17:15 GMT 2025) -----
----- Attempting Submission 4 (Wed Apr 16 21:31:27 GMT 2025) -----
----- Attempting Submission 5 (Mon Apr 28 21:32:49 GMT 2025) -----
----- Attempting Submission 6 (Fri Jun 06 23:11:35 GMT 2025) -----
The frequency and bulk composition of terrestrial exoplanets across Galactic history
Chemically- and kinematically-distinct stellar populations, the thin disk, thick disk, and halo, record the assembly of the Milky Way. It is expected, but not confirmed, that their chemical variation affects planet formation and composition. It is challenging to investigate this using main sequence stars, as known exoplanets overwhelmingly reside in the thin disk, and measuring their occurence rate and compositions is essentially impossible. Metal-polluted white dwarfs, by contrast, not only allow the sensitive detection of planetary systems, but also give access to their bulk compositions. We will obtain UV spectra of a kinematically-selected sample of thick disk and halo white dwarfs using COS. We will then measure (or place stringent limits on) the abundances of rock-forming elements polluting their photospheres. Combining these with a sample of well-characterised thin-disk white dwarfs from archival HST observations, we will be able to measure (1) the frequency of planet formation, and (2) exoplanet iron and water mass fractions, and determine whether these quantities vary across Galactic history, as is theorised.
Technical Set-up: We propose to use the G130M grating in the FUV module with a central wavelength of 1291 A. In accordance with the COS2025 policies, we will only use two FP-POS positions (3 and 4).
COS safety: Our targets are all sufficiently faint that COS safety is not a problem.
CVZ: A few of our targets are located in the continuous viewing zone, but we do not require continuous, uninterrupted observations. Using the visit planner tool, we find that all our targets are schedulable.
Reduced gyro observations: Our observations are not time critical, and can be scheduled any time, so reducing the possible observing windows will not affect this proposal. Using the visit planner tool, there are plenty of schedulable opportunities across the cycle for all targets. Target acquisition is required for all of our targets in order to sucessfully complete the proposed observations.
Scheduling: For targets which require >3 orbits, we have split the visits up to ensure maximum schedulability.
SNR: We require a SNR of >15 around 1330A, close to important lines of carbon.
Our team members have been PI and Co-I on numerous successful HST proposals related to white dwarfs. All team members have experience with and knowledge of observations of white dwarfs and their planetary systems and will all be of valuable help with the analysis. Everyone will contribute to the analysis of the data and the preparation of the publications resulting from this proposal. Laura Rogers, Andrew Swan, Roberto Raddi, Alberto Rebassa, Boris Gaensicke, and Siyi Xu have extensive knowledge and experience with the reduction and analysis of spectroscopic data of white dwarfs. Lou Baya Ould Rouis and Roberto Raddi are experts in mapping white dwarfs with galactic locations. Edward Young, Isabella Trierweiler, and Andrew Buchan are experts in the understanding and interpretation of the composition and geology of exoplanetary material inferred from polluted white dwarfs. Boris Gaensicke is an expert on atmospheric models of white dwarfs and will fit models to the obtained FUV spectra in order to get updated white dwarf parameters, and the abundances of the exo-planetary material that have polluted the atmospheres of the white dwarfs.
Exoplanets and Exoplanet Formation
6
false
true
false
false
false
false
SUPPORTED
STAR
DA
NO
J2000
J2000
FUV=14.96
STAR
DA
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J2000
J2000
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STAR
DA
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DA
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DA
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DA
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DA
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DA
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DA
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STAR
DA
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DA
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DA
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DA
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DA
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DA
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DA
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DA
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DA
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The scheduling data was generated by CASM 33.0.
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