Calibrating the Mass-Luminosity Relation at the End of the Main Sequence

Details Calibrating the Mass-Luminosity Relation at the End of the Main Sequence Calibrating the Mass-Luminosity Relation at the End of the Main Sequence

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8292h&link_type=abstract

HST Proposal ID #8292

Physics

Hst Proposal Id #8292 Cool Stars

Scientific paper

This is a continuation request for GO 6047/6566/7493. We will use HST-FGS1R to calibrate the mass-luminosity relation {MLR} for stars less massive than 0.2 Msun, with special emphasis on objects near the stellar/brown dwarf border. Our goals are to determine M_V values to 0.10 magnitude, masses to 5%, and more than double the number of objects with masses determined to be less than 0.20 Msun. This program uses the combination of HST-FGS3/FGS1R at optical wavelengths and ground-based infrared speckle work to examine nearby, subarcsecond binary systems. Several of the objects included have M < 0.1 Msun, placing them at the very end of the stellar main sequence, and making them brown dwarf candidates.

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