Mass ratio of the 2 pc binary brown dwarf LUH16 and limits on planetary companions from astrometry
Sahlmann et al
We analyse FORS2/VLT I-band imaging data to monitor the motions of both components in the most nearby known binary brown dwarf WISE J104915.57-531906.1AB (LUH16) over one year. The astrometry is dominated by parallax and proper motion, but with a precision of ∼0.2 milli-arcsecond per epoch we accurately measure the relative position change caused by the orbital motion of the pair. This allows us to directly determine a mass ratio of q=0.78±0.10 for this system. We also search for the signature of a planetary-mass companion around either of the A and B component and exclude at 3-σ the presence of planets with masses larger than 2MJup and orbital periods of 20-300 d. We update the parallax of LUH16 to 500.51±0.11 mas, i.e. just within 2 pc. This study yields the first direct constraint on the mass ratio of LUH16 and shows that the system does not harbour any close-in giant planets.
Friday, July 31, 2015
No "hot" Jupiters Around Brown Dwarf Binary Luhman 16AB
Posted by Will Baird at 8:00 AM
Labels: close-in exoplanets, hot jupiters, hot neptunes, luhman 16, luhman 16AB, photometry, VLT
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