The Masses of the Brown Dwarf Candidate GL 623B and of the Low Luminosity Binary GL 831

Details The Masses of the Brown Dwarf Candidate GL 623B and of the Low Luminosity Binary GL 831 The Masses of the Brown Dwarf Candidate GL 623B and of the Low Luminosity Binary GL 831

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7491f&link_type=abstract

HST Proposal ID #7491

Astronomy and Astrophysics

Astronomy

Hst Proposal Id #7491 Cool Stars

Scientific paper

Astrometry at 1-mas accuracy of faint companions to nearby M-dwarfs is the most productive direct method to determine accurate masses of stars near the end of the main sequence. In Cycle 4 we achieved first confirmed detection at visible wavelengths of the astrometric companions of GL 623 and GL 831 with FGS in TRANS mode {Franz et al. 1994}. In Cycle 5 we began observations with FGS in POS/TRANS mode in order to determine, with milli-arcsec accuracy, the motions of the individual components relative to proximate reference stars. Such measures will yield component masses free of assumptions and with an expected accuracy of 5 percent. From preliminary FGS results we estimate the mass of GL 831B as 0.12 solar masses and that of GL 623B as 0.10 solar masses, placing both near the stellar/substellar border. While Cycle 6 observations should suffice to define the orbits and mass ratios, the Cycle 7 observations will be necessary and sufficient to separate barycentric, parallactic, and proper motions of the binary components with the 1-mas precision required to yield masses accurate to about 5 percent. Such a mass determination for GL 623B should establish conclusively its nature as star or substellar object.

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