Determining the Binary Frequency for Ultra-cool, Nearby M Dwarfs

Details Determining the Binary Frequency for Ultra-cool, Nearby M Dwarfs Determining the Binary Frequency for Ultra-cool, Nearby M Dwarfs

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6345k&link_type=abstract

HST Proposal ID #6345

Computer Science

Hst Proposal Id #6345 Cs

Scientific paper

The binary frequency for late-M dwarfs is unknown because a survey for companions to these low luminosity objects is difficult due to ground-based limitations. This knowledge has a direct influence on our understanding of star formation processes and on our interpretation of the faint end of the stellar luminosity function. We propose a search around 11 very late M dwarfs {spectral types of M8 V or cooler} to look for stellar and substellar companions at separations from 2 to 1000 AU { 0.2 to 100 arcsec}. Because our targets are within 10 pc, possible companions will {1} be easily verified because they must share common proper motion with the primaries and {2} be easily characterized since their distance is known a priori from the trigonometric parallax of the primary. Based on the observed multiplicity of early- to mid-M dwarfs, these HST observations are expected to discover three to four new, extremely low-luminosity members of the solar neighborhood.

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