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We present $^{12}$CO(2-1) line and 1300 $\mu$m continuum observations madewith the Submillimeter Array (SMA) of the young star DG Tau B. We find, in thecontinuum observations, emission arising from the circumstellar disksurrounding DG Tau B. The $^{12}$CO(2-1) line observations, on the other hand,revealed emission associated with the disk and the asymmetric outflow relatedwith this source. Velocity asymmetries about the flow axis are found over theentire length of the flow. The amplitude of the velocity differences is of theorder of 1 -- 2 km s$^{-1}$ over distances of about 300 -- 400 AU. We interpretthem as a result of outflow rotation. The sense of the outflow and diskrotation is the same. Infalling gas from a rotating molecular core cannotexplain the observed velocity gradient within the flow. Magneto-centrifugaldisk winds or photoevaporated disk winds can produce the observed rotationalspeeds if they are ejected from a keplerian disk at radii of several tens ofAU. Nevertheless, these slow winds ejected from large radii are not verymassive, and cannot account for the observed linear momentum and angularmomentum rates of the molecular flow. Thus, the observed flow is probablyentrained material from the parent cloud. DG Tau B is a good laboratory tomodel in detail the entrainment process and see if it can account for theobserved angular momentum.

Kinematics of the Outflow From The Young Star DG Tau B: Rotation in the vicinities of an optical jet