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 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001hst..prop.9234h&link_type=abstract

HST Proposal ID #9234

Physics

Hst Proposal Id #9234

Scientific paper

This is a continuation of GO 6047/6566/7493/8282/8774. We 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 Mv 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-FGS3/1R 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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