The molecular kinematics in the Rho Ophiuchi complex are examined. Streaming motions in the form of V(LSR) gradients along filament axes, as predicted for a shocked cloud model, are found only in a short warm filament associated with L1689N, but are not found in the three longest filaments. They have, instead, either approximately uniform V(LSR) or abrupt jumps in V(LSR) between adjacent lumps. A small fraction of clumps are rotating. About evenly divided between senses of rotation, most of these clumps share a common axial alignment paralleling the ambient magnetic field. Within most individual clumps the V(LRSR) is constant within 0.1-0.2 km/s. There is no correlation between the turbulent velocity dispersion in a clump and the clump size or mass. A distinction in turbulent sigma is found between clumps with embedded stars and those without.
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R. B. Loren (1989) studied this question.