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Spatially-resolved velocity maps at high resolutions of 1-10 pc are becomingavailable for many nearby AGNs in both optical/infrared atomic emission linesand sub-mm molecular lines. For the former, it has been known that a linearrelationship appears to exist between the velocity of the ionized gas cloudsand the distance from the nucleus in the inner ~100 pc region, where theseclouds are outflowing. Here we demonstrate that, in such a case, we canactually derive the three-dimensional (3D) geometrical distribution of theclouds directly from the velocity map. Revisiting such a velocity map taken byHST for the prototypical Type 2 AGN NGC1068, we implement the visualization ofthe 3D distribution derived from the map, and show that this inner narrow-lineregion has indeed a hollow-cone structure, consistent with previous modelingresults. Quite possibly, this is the outer extended part of the polar elongateddusty material seen in the recent mid-IR interferometry at pc scale.Conversely, the latter small-scale geometry is inferred to have a hollow-coneoutflowing structure as the inward extension of the derived 3D distributionabove. The AGN obscuring "torus" is argued to be the inner optically thick partof this hollow-cone outflow, and its shadowed side would probably be associatedwith the molecular outflow seen in certain sub-mm lines. We discuss the natureof the linear velocity field, which could be from an episodic acceleration thathad occurred ~10^5 years ago.

Velocity-inverted three-dimensional distribution of the gas clouds in the Type 2 AGN NGC1068