  The role of bipolar jets in the formation of stars, and in particular how
they are launched, is still not well understood. We probe the protostellar jet
launching mechanism, via high resolution observations of the near-IR [FeII]
1.53,1.64 micron lines. We consider the bipolar jet from the Classical T Tauri
star, DO Tau, & investigate jet morphology & kinematics close to the star,
using AO-assisted IFU observations from GEMINI/NIFS. The brighter, blue-shifted
jet is collimated quickly after launch. This early collimation requires the
presence of magnetic fields. We confirm velocity asymmetries between the two
jet lobes, & confirm no time variability in the asymmetry over a 20 year
interval. This sustained asymmetry is in accordance with recent simulations of
magnetised disk-winds. We examine the data for jet rotation. We report an upper
limit on differences in radial velocity of 6.3 & 8.7 km/s for the blue &
red-shifted jets, respectively. Interpreting this as an upper limit on jet
rotation implies that any steady, axisymmetric magneto-centrifugal model of jet
launching is constrained to a launch radius in the disk-plane of 0.5 & 0.3 au
for the blue & red-shifted jets, respectively. This supports an X-wind or
narrow disk-wind model. This pertains only to the observed high velocity [FeII]
emission, & does not rule out a wider flow launched from a wider radius. We
report detection of small amplitude jet axis wiggling in both lobes. We rule
out orbital motion of the jet source as the cause. Precession can better
account for the observations but requires double the precession angle, & a
different phase for the counter-jet. Such non-solid body precession could arise
from an inclined massive Jupiter companion, or a warping instability induced by
launching a magnetic disk-wind. Overall, our observations are consistent with
an origin of the DO Tau jets from the inner regions of the disk.
