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Assigned ID: 966
----- Attempting Submission 1 (Fri Mar 06 23:58:23 GMT 2020) -----
Updated ORIENT constraints for Visit 51 (repeat of 01).
185343194
----- Attempting Submission 1 (Wed Jul 01 07:31:24 GMT 2020) -----
HST Phase II Proposal 16268 successfully submitted.
Receipt: # 16268-1
----- Attempting Submission 2 (Sat Nov 07 22:58:05 GMT 2020) -----
----- Attempting Submission 3 (Mon Nov 09 17:34:47 GMT 2020) -----
----- Attempting Submission 4 (Tue Mar 16 14:35:11 GMT 2021) -----
----- Attempting Submission 5 (Fri May 07 14:32:02 GMT 2021) -----
----- Attempting Submission 6 (Fri Oct 14 17:37:12 GMT 2022) -----
Resolving Mass Benchmarks for Ultracool Atmospheres
The atmospheres of low-mass stars and brown dwarfs have cool temperatures that foster abundant molecules, complex chemical and dynamical processes, and poorly understood condensate clouds. Developing accurate models of these atmospheres is critical for a wide range of problems, from interpreting the spectra of directly imaged planets to accurate modeling of the long-term evolution of the lowest-mass planetary systems. Despite increasing theoretical sophistication, evaluating the accuracy of these models has been long been limited by the lack of objects with well-determined fundamental properties.
We propose to obtain spatially-resolved optical and IR spectra for a unique sample of ultracool dwarf binaries (M7-T5 spectral types) that have high-precision dynamical masses for the individual components (30-100 Jupiter masses), derived from more than decade of orbit monitoring. Mass measurements break degeneracies between poorly known model parameters, such as those governing cloud formation and fundamental properties like surface gravity. Our HST spectra for this sample of binary systems will establish the gold standard for studies of ultracool atmospheric physics. This is the only sample of ultracool binaries that are resolvable by HST (and JWST in the future) that have precisely measured component masses.
For each of our targets, we'll use one visit to obtain WFC3-IR slitless grism data with both G102 and G141 gratings. For a subset of our targets we will use a separate visit to obtain STIS low-resolution spectra. Separating the visits allows more flexibility in the roll angle constraints needed to make the binary components orthogonal to the dispersion axes of the two different instruments. All of our targets require only one orbit per visit, except for J0423 and J2252 that require two orbits for their STIS spectra.
Dr. Katelyn Allers is an expert on the spectra of ultracool dwarfs and their empirical classification, especially the influence of surface gravity.
Dr. Brendan Bowler has extensive experience with ultracool dwarfs and expertise obtaining HST/WFC3-IR spectra of companions that are challenging to spatially resolve (from data reduction experience with his program HST-GO-15197). His group is developing the software needed for deblending our grism spectra.
Dr. Trent Dupuy has expertise on dynamical masses of ultracool dwarfs, astrometry, testing evolutionary and atmospheric models and the binaries in this proposal. He led the work that developed the proposed sample with adaptive optics imaging and HST data.
Dr. Michael Line is an expert on the retrievals approach to modeling ultracool atmospheres and has developed code for fitting HST WFC3-IR data with a mass prior.
Dr. Michael Liu is an expert on ultracool atmospheres and dynamical masses of brown dwarfs and was a key contributor in developing the proposed sample.
Drs. Mark Marley and Caroline Morley are leading theorists on modeling ultracool atmospheres and will be able provide the latest grid models for use in our analysis.
Mr. Zhoujian Zhang is a graduate student working with Drs. Liu and Marley of grid-based modeling approaches for ultracool dwarfs using the state-of-the-art Sonora models from Marley, Saumon, Fortney, Morley, et al.
Stellar Physics and Stellar Types
Exoplanets and Exoplanet Formation
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true
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The scheduling data was generated by CASM 30.3.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 30.3.
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