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The role of bipolar jets in the formation of stars, and in particular howthey are launched, is still not well understood. We probe the protostellar jetlaunching 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 Tauristar, DO Tau, & investigate jet morphology & kinematics close to the star,using AO-assisted IFU observations from GEMINI/NIFS. The brighter, blue-shiftedjet is collimated quickly after launch. This early collimation requires thepresence of magnetic fields. We confirm velocity asymmetries between the twojet lobes, & confirm no time variability in the asymmetry over a 20 yearinterval. This sustained asymmetry is in accordance with recent simulations ofmagnetised disk-winds. We examine the data for jet rotation. We report an upperlimit 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 jetrotation implies that any steady, axisymmetric magneto-centrifugal model of jetlaunching is constrained to a launch radius in the disk-plane of 0.5 & 0.3 aufor the blue & red-shifted jets, respectively. This supports an X-wind ornarrow 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. Wereport detection of small amplitude jet axis wiggling in both lobes. We ruleout orbital motion of the jet source as the cause. Precession can betteraccount for the observations but requires double the precession angle, & adifferent phase for the counter-jet. Such non-solid body precession could arisefrom an inclined massive Jupiter companion, or a warping instability induced bylaunching a magnetic disk-wind. Overall, our observations are consistent withan origin of the DO Tau jets from the inner regions of the disk.

Launching the asymmetric bipolar jet of DO Tau