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 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005hst..prop10613h&link_type=abstract

HST Proposal ID #10613

Computer Science

Hst Proposal Id #10613 Cool Stars

Scientific paper

We propose to 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 0.05 magnitude, masses to 5 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 interferometry to examine nearby, subarcsecond binary systems. The high precision measurements with HST-FGS3/FGS1R {to 1 mas in the separations} for these faint targets {V = 10-15} simply cannot be equaled by any ground based technique. As a result of these measurements, we are deriving high quality luminosities and masses for the components in the observed systems, and characterizing their spectral energy distributions from 0.5 to 2.2 Mum. Several of the objects included have M < 0.1 Msun, placing them at the very end of the stellar main sequence. Three of the targets are brown dwarf candidates, including the current low mass record holder, GJ 1245C, with a mass of 0.062 +/- 0.004 Msun. The payoff of this proposal is high because all 10 of the systems selected have already been resolved with HST- FGS3/FGS1R during Cycles 5-10 and contain most of the reddest objects for which masses can be determined.

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