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^+0.27 _-0.08 M _⊙ and M ₂ = 0.33^+0.09 _-0.02 M _⊙ 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 PMS stars.