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Optical observations cannot resolve the structure of active galactic nuclei(AGN), and a unified model for AGN was inferred mostly from indirect methods.Optical reverberation mapping allowed us to constrain the spatial dimension ofthe broad emission line region and thereby to measure the mass of supermassiveblack holes. Recently, reverberation was also applied to the polarized signalemerging from different AGN components. In principle, this should allow us tomeasure the spatial dimensions of the sub-parsec reprocessing media. We modeledscattering-induced polarization and tested different geometries for thecircumnuclear dust component. Our tests included the effects of clumpiness anddifferent dust prescriptions. To further extend the model, we also explored theeffects of additional ionized winds stretched along the polar direction, and ofan equatorial scattering ring that is responsible for the polarization angleobserved in pole-on AGN. The simulations were run using a time-dependentversion of the {\sc stokes} code. Our modeling confirms the previously foundpolarization characteristics as a function of the observer`s viewing angle.When the dust adopts a flared-disk geometry, the lags reveal a clear differencebetween type 1 and type 2 AGN. This distinction is less clear for a torusgeometry where the time lag is more sensitive to the geometry and optical depthof the inner surface layers of the funnel. The presence of a scatteringequatorial ring and ionized outflows increased the recorded polarization timelags, and the polar outflows smooths out dependence on viewing angle. Togetherwith other AGN observables, the polarization time lag places new, independentconstraints on the inner geometry of AGN. If we conduct time-dependentspectropolarimetric observing campaigns of AGN, this method has a highpotential for a census of supermassive black holes.

Modeling optical and UV polarization of AGNs