0Assigned ID: 512
----- Attempting Submission 1 (Fri Mar 06 15:53:45 GMT 2020) -----
HST Phase I Proposal 512 successfully submitted.
Receipt: # 512-1
----- Attempting Submission 2 (Fri Mar 06 16:53:39 GMT 2020) -----
HST Phase I Proposal 512 successfully submitted.
Receipt: # 512-2
----- Attempting Submission 3 (Fri Mar 06 17:03:05 GMT 2020) -----TOO MANY SUBEXPOSURES IN ONE GROUP (REQUEST HELP FROM YOUR PC)
TOO MANY SUBEXPOSURES IN ONE GROUP (REQUEST HELP FROM YOUR PC)
TOO MANY SUBEXPOSURES IN ONE GROUP (REQUEST HELP FROM YOUR PC)correct the exposure configuration to be the same as GO-13280-1901263940----- Attempting Submission 1 (Tue Jun 30 02:21:25 GMT 2020) -----
----- Attempting Submission 2 (Thu Sep 24 00:46:53 GMT 2020) -----the subgroup number of 510 exposures is larger than the maximum limit (400). To maximize our science goal, it is important to have a non-interrupted observation within each vist.Bands of brothers: detecting banded structures in the atmospheres of Luhman 16A and BTo date three brown dwarfs in the L/T transition show signs of planetary-wave light-curve beating. Here, the differential rotation of wave-derived structure in various latitudinal bands causes their individual light curves alternately to constructively and destructively interfere. Luhman 16AB is an intriguing target, with both components exhibiting peculiar behaviors that hint to the existence of bands in their atmospheres. Recently, indirect evidence for bands on Luhman 16A were found using polarization. However, no data exists to date that is able to verify the existence of bands on 16A or B. We propose to observe Luhman 16AB with WFC3 to test the existence of bands in these two L/T transition brown dwarfs. Our observations will 1) test the hypothesis that there are planetary-scale waves and bands in L/T transition atmospheres, 2) verify the ability of polarization to detect bands in exoatmospheres, and 3) nearly double the sample of long-temporal-baseline observations available to detect planetary-scale waves in L/T transition brown dwarfs.Our main goal is to observe the light curve evolution of Luhman 16A and B across different rotations with time-series spectroscopy in WFC3/IR/G141 grism mode. At the beginning of each orbit, we obtain a direct image in F132N for wavelength calibration of G141 images. We restrict the orientation range so that the dispersed spectra of the two objects will be at about ~7 pixels away from each other. To obtain a continuous baseline for monitoring the light curve evolution, we require the separation between visits to be less than or equal to two HST orbits.
One of the science goals of our program involves verifying the ability of polarization to detect banded structures in exoatmospheres. To maximize our science case we aim to acquire ground based polarimetric observations nearly simultaneous with the HST observations. We would therefore like to ask that our observations take place in a time when that is possible, namely in order of preference, in April, May-June.Dr. Theodora Karalidi (PI, University of Central Florida) is an expert on spectropolarimetric modelling (Millar-Blancher, Girard, Karalidi et al, 2020) and mapping of brown dwarf atmospheres using Spitzer and HST light curves (Karalidi et al 2015; Apai, Karalidi et al 2017). She will lead the scientific interpretation of the data, including radiative transfer modelling and mapping of the atmospheres, as well as coordinate planning and data reduction, lead publication of results, and manage the overall program. Dr. Daniel Apai was the PI of the Extrasolar Storms (GO 13176) and Cloud Atlas Treasury program (GO 14241), and he is an expert on HST/WFC3 data reduction, analysis, and physical interpretation of the results. Ben Lew is an expert on data reduction of HST/WFC3 data, and in the interpretation of brown dwarfs and exoplanet variability (Lew et al 2016, 2020). Dr Apai and Mr Lew will lead the data reduction and contribute to analysis and scientidic interpretation of the results. Dr. Joseph Harrington is the PI of the Bayesian Atmospheric Radiative Transfer (BART) code. He will lead the retrieval of the Luhman 16A and B properties with BART and contribute to the scientific interpretation of the results. Dr. Mark Marley and Dr. Xi Zhang are experts on radiative transfer modelling and General Circulation Models of brown dwarfs and giant planets respectively. They will contribute to the scientidic interpretation of the results. Dr. Max Millar-Blanchaer is an expert on polarimetric observations of direct imaged exoplanets. He will contribute to the scientidic interpretation of the results.Stellar Physics and Stellar TypesExoplanets and Exoplanet Formation6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARBROWN DWARFThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARBROWN DWARFbased on Rolly's astrometric solution 162.299250316 -53.317213006 on JD=2459707.500000000J2000WFC3/IRSpectroscopicNoNoG141Timing link suitability includes constraints ([02 After 01 by 0.3 to 0.5 days] [R2 After 01 by 0.3 to 0.5 days])Hst Same orient constraint links visits (01 02 03)The scheduling data was generated by CASM 29.0.CASM was run in Phase II mode.PA from Luhman 16A to B = 131 deg (north to east) at ~2021.5
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