  We present an updated analysis of LHS 6343, a triple system in the Kepler
field which consists of a brown dwarf transiting one member of a
widely-separated M+M binary system. By analyzing the full Kepler dataset and 34
Keck/HIRES radial velocity observations, we measure both the observed transit
depth and Doppler semiamplitude to 0.5% precision. With Robo-AO and
Palomar/PHARO adaptive optics imaging as well as TripleSpec spectroscopy, we
measure a model-dependent mass for LHS 6343 C of 62.1 +/- 1.2 M_Jup and a
radius of 0.783 +/- 0.011 R_Jup. We detect the secondary eclipse in the Kepler
data at 3.5 sigma, measuring e cos omega = 0.0228 +/- 0.0008. We also derive a
method to measure the mass and radius of a star and transiting companion
directly, without any reliance on stellar models. The mass and radius of both
objects depend only on the orbital period, stellar density, reduced semimajor
axis, Doppler semiamplitude, eccentricity, and inclination, as well as the
knowledge that the primary star falls on the main sequence. With this method,
we calculate a model-independent mass and radius for LHS 6343 C to a precision
of 3% and 2%, respectively.
