  We analyze radial velocities for a sample of 31 Class I and flat spectrum
protostars in Taurus-Auriga, rho Ophiuchi and Serpens for evidence of the
global dynamical state of extremely young stellar populations buried within
parental molecular clouds. Comparing the radial velocity of each protostar to
that of the local CO gas, we are able to constrain the one dimensional radial
velocity dispersion of Class I and flat spectrum objects to ~ 2.5 km/sec or
below. This upper limit to the protostellar velocity dispersion is consistent
with the velocity dispersions of surrounding CO gas which we measure to be ~
1.4 km/sec, suggesting that the motions of protostars and local CO gas are
dynamically linked and dominated by the gravitational potential of the
molecular cloud. However, the upper limit on the protostellar velocity
dispersion could still allow for slightly inflated motions of protostars
relative to the local molecular gas. Four of the protostars analyzed appear to
have velocities more than 3 sigma (7.5 km/sec) away from the central local CO
gas velocity while showing spectroscopic indicators of youth and accretion such
as H_2 emission, HI Br Gamma emission, or K band continuum veiling. These
radial velocity outliers may represent protostellar spectroscopic binaries or
ejected cluster members.
