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We present new orbital measurements of the pre-main sequence triple system,V807 Tau, using adaptive optics imaging at the Keck Observatory. We computed anorbit for the close pair, V807 Tau Ba-Bb, with a period of 12.312 +/- 0.058years and a semi-major axis of 38.59 +/- 0.16 mas. By modeling the center ofmass motion of the components in the close pair relative to the wide component,V807 Tau A, we measured a mass ratio of 0.843 +/- 0.050 for Bb/Ba. Combinedwith the total mass from the relative orbit, we derived individual masses ofM_Ba = 0.564 +/- 0.018 (d/140 pc)^3 Msun and M_Bb = 0.476 +/- 0.017 (d/140pc)^3 Msun at an average distance of 140 pc to the Taurus star forming region.We computed spectral energy distributions to determine the luminosities of thethree components. We also measured their spectral types, effectivetemperatures, and rotational velocities based on spatially resolved spectraobtained at the Keck Observatory. If the rotational axes are aligned, then theprojected rotational velocities imply that V807 Tau Ba and Bb are rotating muchfaster than V807 Tau A. The uncertainty in the stellar effective temperaturesand distance to the system currently limit the comparison of our dynamical massmeasurements with predictions based on evolutionary tracks for pre-mainsequence stars. We also report preliminary results from a program to map the3.6 cm radio emission from V807 Tau using the Very Long Baseline Array. Withcontinued monitoring, these observations will provide a precise parallax forplacing the dynamical masses on an absolute scale.

Orbit and Stellar Properties of the Young Triple V807 Tau