Preliminary Orbit of the Young Binary Haro 1-14c

Using the Keck Interferometer, we spatially resolved the orbit of the pre-main-sequence (PMS) 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(-0.08)(+0.27) M-circle dot and M-2 = 0.33(-0.02)(+0.09) M-circle dot for the primary and secondary, respectively, and a distance to the system of 111(-18)(+19) 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 PMS stars.