  Using the Keck Interferometer, we spatially resolved the orbit of the
pre-main sequence binary, Haro 1-14c, for the first time. We present these
interferometric observations along with additional spectroscopic radial
velocity measurements of the components. We performed a simultaneous orbit fit
to the interferometric visibilities and the radial velocities of Haro 1-14c.
Based on a statistical analysis of the possible orbital solutions that fit the
data, we determined component masses of M_1 = 0.96 (+0.27/-0.08) Msun and M_2 =
0.33 (+0.09/-0.02) Msun for the primary and secondary, respectively, and a
distance to the system of 111 (+19/-18) pc. The distance measurement is
consistent with the close distance estimates of the Ophiuchus molecular cloud.
Comparing our results with evolutionary tracks suggests an age of 3-4 Myr for
Haro 1-14c. With additional interferometric measurements to improve the
uncertainties in the masses and distance, we expect the low-mass secondary to
provide important empirical data for calibrating the theoretical evolutionary
tracks for pre-main sequence stars.
