PI: S Mark Ammons, Lawrence Livermore National Laboratory, email@example.com
Address: Livermore, CA, 94551-9900 USA
CoI: Christian Marois, Herzberg Institute of Astrophysics
CoI: GPIES team GPIES team, Stanford U.
CoI: Quinn Konopacky, UC San Diego
CoI: Benoit Neichel, Laboratoire d'Astrophysique de Marseille
Title: The Best Parallaxes and a Limit on the Giant Planet Occurrence Rate for Nearby T Dwarf Hosts
Abstract: We propose to continue an astrometric monitoring program on ten of twenty T dwarfs currently being monitored with Gemini GeMS, Keck NIRC2, and ShaneAO at Lick Observatory. Seven have been observed by HST WFC3 in 2010. The targets have been selected from WISE’s sample of brown dwarfs (Kirkpatrick et al. 2011), the UKIDSS Large Area Survey (Lawrence et al. 2012) and the UKIDSS Galactic Plane Survey (Lucas et al. 2012). The T dwarfs we observe are too optically faint to be targeted by existing optical radial velocity (RV) instruments or GAIA. Combined with HST WFC3 observations in 2010 and continuing ShaneAO observations in 2016, the proposed observations will lead to < 1% trigonometric distances for the entire sample, enabling precision luminosity measurements, and obtain 0.3-1.0 MJUP limits with 0.2 < P < 6 years. In the case of no detections, the giant planet occurrence rate for T dwarfs could be shown to be distinct from that of FGK stars (Johnson et al. 2010) at the 3-sigma level, which would suggest that the trend of increasing giant planet frequency with stellar mass holds at the low mass end.
Program Type: Standard/Galactic
Run 1 (2016B): GEM-SQ/GSAOI -- 7hrs band 2 (GS-2016B-Q-32)
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