  Spatially resolving the orbits of double-lined spectroscopic binaries
provides a way to measure the dynamical masses of the component stars. At the
distances to the nearest star forming regions, high angular resolution
techniques are required to resolve these short period systems. In this paper, I
provide an overview of the few low-mass pre-main-sequence spectroscopic
binaries that have been resolved thus far using long-baseline optical/infrared
interferometers. I also compiled a list of known spectroscopic binaries in
nearby star forming regions (Taurus, Orion, Ophiuchus, Scorpius-Centaurus,
etc.) and show that with modest improvements in the sensitivity of
interferometers with 200-300 meter baselines, we can build a significant set of
pre-main sequence stars with precise mass determinations. This is important for
validating and distinguishing among the theoretical calculations of evolution
for young stars.
