  We present results from high resolution optical spectra toward 66 young stars
in the Orion B molecular cloud to study their kinematics and other properties.
Observations of the H$\alpha$ and Li I 6707 {\AA} lines are used to check
membership and accretion properties. While the stellar radial velocities of in
NGC 2068 and L1622 show good agreement with that of the molecular gas, many of
the stars in NGC 2024 show a considerable offset. This could be a signature of
either expansion of the cluster, high degree of the ejection of the stars from
the cluster through the dynamical interaction, or the acceleration of the gas
due to stellar feedback.
