High Precision Dynamical Masses of M, L, and Brown Dwarf Binaries with Aperture Masking Interferometry

Details High Precision Dynamical Masses of M, L, and Brown Dwarf Binaries with Aperture Masking Interferometry High Precision Dynamical Masses of M, L, and Brown Dwarf Binaries with Aperture Masking Interferometry

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21340614b&link_type=abstract

American Astronomical Society, AAS Meeting #213, #406.14; Bulletin of the American Astronomical Society, Vol. 41, p.201

Astronomy and Astrophysics

Astronomy

Scientific paper

The theoretical relations that determine stellar age, mass, and metallicity from astronomical observations (luminosity and color) are largely untested for M, L, and brown dwarfs. Previous results of our group suggest these models are inaccurate. Correctly calibrating these models is extremely important for their effectiveness, especially as these models are extended to the masses of brown dwarfs and giant extra-solar planets. Thus, the planetary status of directly imaged extra-solar planets and the masses of brown dwarfs remain model dependent.
Dynamical mass measurements of star systems, which are model independent, are by far the most effective observations for challenging and improving these stellar models. This is the motivation for Aperture Masking.
Aperture Masking is a robust observational technique that allows the detection of high contrast companions (>300:1) at distances closer than the formal diffraction limit ( 0.6 L/D). The mask, transmitting through a sparsely populated set of small holes, converts the telescope mirror into a makeshift interferometer without sacrificing precise photometry.
We are currently using Aperture Masking to find companions and dynamical masses to twenty-five M dwarfs and forty L dwarfs. Our group also recently completed a survey of Upper Scorpius, searching for low mass companions in the so-named "brown dwarf desert.” Our results and a description of our technique are presented here.

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