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Paper: M and L Dwarf Dynamical Masses with One Adaptive Optics Observation
Volume: 448, 16th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun
Page: 849
Authors: Dieterich, S. B.; Henry, T. J.; Jao, W.-C.; Riedel, A. R.
Abstract: The accurate determination of individual dynamical masses is crucial for a comprehensive understanding of objects at the end of the stellar main sequence. As a part of our efforts to thoroughly characterize the stellar/substellar transition region, we have recently begun an effort to obtain dynamical masses for individual components of sub-arcsecond M and L dwarf binaries. Our method combines photocentric orbits obtained as a bi-product of trigonometric parallax observations at CTIO with a single Gemini North / NIRI AO resolved image. The separation and flux ratio of the AO image is then used to scale the photocentric orbit into the barycentric orbit necessary to solve Kepler's third law. Because the photocentric orbit is measured relative to the background of “fixed” stars, this method also yields the mass ratio of the two components. We describe our methodology and mention the current state of the project in these proceedings.
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