Science Keywords: Brown Dwarfs is not a valid selection.0Assigned ID: 111
----- Attempting Submission 1 (Wed Apr 03 00:54:47 GMT 2019) -----APT is whining about keywords... but we are searching exoplanets around BDs. Brett told us we can ignore this problem and submit it. :)FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser0----- Attempting Submission 1 (Mon Jul 08 09:10:51 GMT 2019) -----
----- Attempting Submission 2 (Thu Nov 05 22:01:04 GMT 2020) -----observations collected as in previous epochsConfirmation of an Astrometrically Detected Exoplanet Candidate Orbiting the closest Brown DwarfsAt a distance of slightly less than 2 pc WISE 1049-5319 (or Luhman 16 AB) is the closest system to Earth after those of alpha Centauri and Barnard's Star.
The analysis of astrometric measurements collected in 12 HST epochs (between 2014.64 and 2016.76) revealed a weak astrometric signature indicating the presence of an exoplanet in the Luh16AB system. This candidate was reported in 2017. A single additional epoch ---collected in August 2018--- and re-analysis of the data with more advanced methods increased the significance level of the planet candidate.
Here we propose to use HST in the same observing mode to collect data at two new epochs to confirm or disprove the astrometric signature that suggest the presence of a sub-Neptune-mass exoplanet orbiting one component of the closest known brown dwarf system. If confirmed, it would be the first astrometrically detected exoplanet around a brown dwarf and the third closest known exoplanet; a major discovery which only requires a relatively modest investment of two additional HST orbits.
The proposed epochs will extend the temporal coverage of the astrometric monitoring to two planet orbital periods (based on the current orbit fits). Coverage over two periods is required to: (a) confirm that our model of the planetary system is predictive, and (b) verify and refine uncertainty estimates. Furthermore, should the orbit be non-circular, these additional measurements will determine this and significantly improve the orbital semi-major axis measurement.Each epoch contains three images in point source imaging mode, and four in spatial-scanning mode with WFC3/UVIS.
In addition to the images taken in spatial scan mode and to the short two point-source images at the beginning and at the end of the
single orbit-visits --- as requested at the phase I stage --- it turned out possible to fit in the orbit one extra point source images of 348s in
F606W. The color information will be a precious to discriminate the nature (and so the distance) of the reference sources in the field
(for example to separate slow close by red dwarf from far away giants)Dr. Luigi Bedin (PI, INAF-OAPD) is an expert on imaging photometry and astrometry with HST under-sampled images, and has contributed to state of the art calibrations and corrections of HST data, linking HST astrometry to the Gaia reference system to achieve sub-mas precisions. Dr. Bedin will coordinate planning and data reduction, contribute to analysis, lead publication of results, and manage the overall program.
Drs. Luigi R. Bedin (Osservatorio Astronomico di Padova) and Mattia Libralato (STScI) have led the development and application of precision astrometric techniques with HST/WFC3 for low-temperature brown dwarfs (Bedin et al. 2017, MNRAS, 470, 1140; Bedin & Fontanive 2018, MNRAS, 481, 5339) and stellar systems (Libralato et al. 2016, MNRAS, 463, 1780). They will lead analysis to extract precision astrometric measurements, and astrometric parameters.
Prof. Adam Burgasser (PI, UCSD) is an expert on the discovery, spectral characterization and multiplicity of the lowest-mass stars and brown dwarfs. He PI'd two successful HST programs examining the multiplicity of T dwarfs (Burgasser et al. 2003, ApJ, 586, 512; 2006; ApJS, 166, 585) and led analysis that first characterized the components of the Luhman16AB system (Burgasser et al. 2013, ApJ, 772, 129). Prof. Burgasser will contribute to the scientific interpretation and analysis of the data.
Prof. Daniel Apai (U. Arizona) is an expert on brown dwarf and exoplanet spectroscopy, leading several HST/WFC3 and ground-based programs examining weather-related variability (Apai et al. 2017, Science, 357, 683) and exoplanet detection (Apai et al 2016, ApJ, 820, 40). Prof. Apai will contribute to the scientific interpretation of the data.Planets and Planet Formation6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARBROWN DWARFNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
This a binary with the two component at ~ 1 arcsec separationWISE1049-5319J2000J2000STARBROWN DWARFWe have mapped the relative path of Luhman 16AB between 2014 and 2016J2000J2000Sloan-i = 15 +/- .5WFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WThe scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.Epoch 2019 OCT.
This is the epoch is taken at the ricciolo of the cycloid apparent motion.
The epoch must be around 2019-10-20 +/- 15 days1571504060000233.23278542116668(Tic-Visit
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)false11The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.Epoch 2021 NOV
This is the epoch is taken at the ricciolo of the cycloid apparent motion.
The epoch must be after 2021-11-01(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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:dark-offset NIL
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