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We map the kinematics of the inner (200 pc) narrow-line region (NLR) of theSeyfert 2 galaxy NGC 1068 using the instrument NIFS and adaptative optics atthe Gemini North Telescope. Channel maps and position-velocity diagrams arepresented at a spatial resolution of $\sim$ 10 pc and spectral resolution$\sim$ 5300 in the emission lines [Fe II] {\lambda} 1.644 {\mu}m, H$_2${\lambda} 2.122 {\mu}m and Br{\gamma}. The [Fe II] emission line provides abetter coverage of the NLR outflow than the previously used [O III] {\lambda}5007 emission line, extending beyond the area of the bi-polar cone observed inBr{\gamma} and [O III]. This is mainly due to the contribution of theredshifted channels to the NE of the nucleus, supporting its origin in apartial ionized zone with additional contribution from shocks of the outflowinggas with the galactic disc. We modeled the kinematics and geometry of the [FeII] emitting gas finding good agreement with the data for outflow models withconical and lemniscate (or hourglass) geometry. We calculate a mass outflowrate $1.9^{+1.9}_{-0.7}$ M$_{\odot}~$yr$^{-1}$ but a power for the outflow ofonly 0.08% L$_{Bol}$. The molecular (H$_2$) gas kinematics is completelydistinct from that of [Fe II] and Br{\gamma}, showing radial expansion in anoff-centered $\sim$ 100 pc radius ring in the galaxy plane. The expansionvelocity decelerates from $\sim$ 200 km/s in the inner border of the ring toapproximately zero at the outer border where our previous studies found a 10Myr stellar population.

Modeling the [Fe II]{\lambda}1.644{\mu}m outflow and comparison with H$_2$ and H$^+$ kinematics in the inner 200 pc of NGC 1068