Velocity-inverted three-dimensional distribution of the gas clouds in
  the Type 2 AGN NGC1068
  Spatially-resolved velocity maps at high resolutions of 1-10 pc are becoming
available for many nearby AGNs in both optical/infrared atomic emission lines
and sub-mm molecular lines. For the former, it has been known that a linear
relationship appears to exist between the velocity of the ionized gas clouds
and the distance from the nucleus in the inner ~100 pc region, where these
clouds are outflowing. Here we demonstrate that, in such a case, we can
actually derive the three-dimensional (3D) geometrical distribution of the
clouds directly from the velocity map. Revisiting such a velocity map taken by
HST for the prototypical Type 2 AGN NGC1068, we implement the visualization of
the 3D distribution derived from the map, and show that this inner narrow-line
region has indeed a hollow-cone structure, consistent with previous modeling
results. Quite possibly, this is the outer extended part of the polar elongated
dusty material seen in the recent mid-IR interferometry at pc scale.
Conversely, the latter small-scale geometry is inferred to have a hollow-cone
outflowing structure as the inward extension of the derived 3D distribution
above. The AGN obscuring "torus" is argued to be the inner optically thick part
of this hollow-cone outflow, and its shadowed side would probably be associated
with the molecular outflow seen in certain sub-mm lines. We discuss the nature
of the linear velocity field, which could be from an episodic acceleration that
had occurred ~10^5 years ago.
