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If the existence of an obscuring circumnuclear region around the innermostregions of active galactic nuclei (AGN) has been observationally proven, itsgeometry remains highly uncertain. The morphology usually adopted for thisregion is a toroidal structure, but other alternatives, such as flared disks,can be a good representative of equatorial outflows. Those two geometriesusually provide very similar spectroscopic signatures, even when they aremodeled under the assumption of fragmentation. In this lecture note, we showthat the resulting polarization signatures of the two models, either a torus ora flared disk, are quite different from each other. We use a radiative transfercode that computes the 2000 - 8000 angstrom polarization of the twomorphologies in a clumpy environment, and show that varying the sizes of atoroidal region has deep impacts onto the resulting polarization, while thepolarization of flared disks is independent of the outer radius. Clumpy flareddisks also produce higher polarization degrees (about 10 % at best) togetherwith highly variable polarization position angles.

The optical polarization signatures of fragmented equatorial dusty structures in Active Galactic Nuclei