Modeling the [Fe II]λ1.644µm outflow and comparison with

We map the kinematics of the inner (200 pc) narrow-line region (NLR) of the Seyfert 2 galaxy NGC 1068 using the instrument NIFS and adaptative optics at the Gemini North Telescope. Channel maps and position-velocity diagrams are presented at a spatial resolution of ∼ = 10 pc and spectral resolution ∼ 5300 in the emission lines [Fe ii]λ 1.644µm, H2 λ 2.122µm and Brγ. The [Fe ii] emission line provides a better coverage of the NLR outflow than the previously used [O iii]λ 5007 emission line, extending beyond the area of the bi-polar cone observed in Brγ and [O iii]. This is mainly due to the contribution of the redshifted channels to the NE of the nucleus, supporting its origin in a partial ionized zone with additional contribution from shocks of the outflowing gas with the galactic disc. We modeled the kinematics and geometry of the [Fe ii] emitting gas finding good agreement with the data for outflow models with conical and lemniscate (or hourglass) geometry. We calculate a mass outflow rate of 1.9+1.9−0.7 M yr −1 but a power for the outflow of only 0.08 % LBol. The molecular (H2) gas kinematics is completely distinct from that of [Fe ii] and Brγ, showing radial expansion in an off-centered ∼ 100 pc radius ring in the galaxy plane. The expansion velocity decelerates from ≈ 200 km s−1 in the inner border of the ring to approximately zero at the outer border where our previous studies found a 10 Myr stellar population