Dr. Gail Schaefer
Haro 1-14c is a pre-main sequence binary star located in the Ophiuchus star forming region. It is a double-lined spectroscopic binary with a period of 591 days. Over the past few years, we used the Keck Interferometer to resolve the system spatially and map its visual orbit. By combining our interferometer observations with published radial velocity measurements, we computed a preliminary orbit and determined the stellar masses and distance to the system. I will provide an overview on measuring the masses of young stars and discuss the implications that the current measurements have on testing theoretical models of stellar evolution for pre-main sequence stars.