  We present new near-IR long slit spectroscopic data obtained with ISAAC on
VLT/ANTU (ESO/Paranal) of the central 4''x 4'' region surrounding the central
engine of NGC1068 . Bracket Gamma (Bg) and H2 emission line maps and line
profile grids are produced, at a spatial resolution~0.5" and spectral
resolution 35km/s. Two conspicuous knots of H2 emission are detected at about
1'' on each side of the central engine along PA=90deg, with a projected
velocity difference of 140km/s: this velocity jump has been interpreted in
Alloin et al (2001) as the signature of a rotating disk of molecular material.
Another knot with both H2 and Bg emission is detected to the North of the
central engine, close to the radio source C where the small scale radio jet is
redirected and close to the brightest [OIII] cloud NLR-B. At the achieved
spectral resolution, the H2 emission line profiles appear highly asymmetric
with their low velocity wing being systematically more extended than their high
velocity wing. A simple way to account for the changes of the H2 line profiles
(peak-shift with respect to the systemic velocity, width, asymmetry) over the
entire 4''x 4'' region, is to consider that a radial outflow is superimposed
over the emission of the rotating molecular disk. We present a model of such a
kinematical configuration and compare our predicted H2 emission profiles to the
observed ones.
