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The recent ALMA maps together with observations of H$_2$O maser emission seemto suggest the presence of a counter-rotation in the obscuring torus of NGC1068. We propose to explain this phenomenon as due to the influence of a wind,considered as radiation pressure, and the effects of torus orientation. Inorder to test this idea: 1. we make $N$-body simulation of a clumpy torustaking into account mutual forces between particles (clouds); 2. we applyray-tracing algorithm with the beams from the central engine to choose theclouds in the torus throat that can be under direct influence of the accretiondisk emission; 3. we use semi-analytical model to simulate the influence of theasymmetrical radiation pressure (wind) forced on the clouds in the torusthroat. An axis of such a wind is tilted with respect to the torus symmetryaxis; 4. we orient the torus relative to an observer and again applyray-tracing algorithm. In this step the beams go from an observer to theoptically thick clouds that allows us to take into account the mutualobscuration of clouds; 5. after projecting on the picture plane, we impose agrid on the resulting cloud distribution and find the mean velocity of cloudsin each cells to mimic the ALMA observational maps. By choosing the parameterscorresponding to NGC 1068 we obtain the model velocity maps that emulate theeffect of an apparent counter-rotation and can explain the discovery made byALMA.

Apparent counter-rotation in the torus of NGC 1068: influence of an asymmetric wind