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 } ~ { } M _ { \odot } and M _ { 2 } = 0.33 ^ { +0.09 } _ { -0.02 } ~ { } M _ { \odot } 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 .