  We present high sensitivity and high angular resolution images of the high
velocity (vLSR>30kms^-1) CO emission in the J=1-0 and J=2-1 lines of the Orion
KL region. These results reveal the morphology of the high-velocity CO emission
at the most extreme velocities. High velocity emission have been only detected
in two regions: BN/KL (IRc2/I) and Orion-S.
  The Orion-S region contains a very young (dynamical age of 10^3years), very
fast (~110kms^-1) and very compact (<0.16pc) bipolar outflow. From the
morphology of the high-velocity gas we estimate that the position of the
powering source must be ~20'' north of FIR4. For the IRc2/I molecular outflow
the morphology of the moderate velocity (<60kms^-1) gas shows a weak bipolarity
around IRc2/I. The gas at the most extreme velocities does not show any
bipolarity around IRc2/I, if any, it is found ~30'' north from these sources.
The blue and redshifted gas at moderate velocities shows similar spatial
distribution with a systematic trend for the size of the high-velocity gas to
decrease as the terminal radial velocity increases. The size-velocity
relationship is fitted with a simple velocity law which considers a highly
collimated jet and entrained material outside the jet moving in the radial
direction. We also find that most of the CO outflowing at moderate velocities
is located at the head of the jet. Our results and the spatial distribution and
kinematics of the shock tracers in this outflow can be explained if the IRc2/I
outflow is driven by a precessing jet oriented along the line of sight.
