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A growing body of evidence suggests that part of, if not all, scatteringregions of active galactic nuclei (AGNs) are clumpy. Hence. in this paper, werun radiative transfer models in the optical/UV for a variety of AGNreprocessing regions with different distributions of clumpy scattering media.We use the latest version of the Monte Carlo code STOKES presented in the firsttwo papers of this series to model AGN reprocessing regions of increasingmorphological complexity. We replace previously uniform-density media with upto thousands of constant-density clumps. We couple a continuum source tofragmented equatorial scattering regions, polar outflows, and toroidal,obscuring dust regions and investigate a wide range of geometries. We alsoconsider different levels of fragmentation in each scattering region toevaluate importance of fragmentation for the net polarization of the AGN. Wefind that, in comparison with uniform-density models, equatorial distributionsof gas and dust clouds result in grayer spectra, and show a decrease of the netpolarization percentage at all lines of sight. The resulting polarizationposition angle depends on the morphology of the clumpy structure, with extendedtori favoring parallel polarization while compact tori produce orthogonalpolarization position angles. In the case of polar scattering regions,fragmentation increases the net polarization unless the cloud filling factor issmall. A complete set of AGN models constructed from the individual, fragmentedregions is investigated. Our modeling shows that the introduction of fragmenteddusty tori significantly alters the resulting net polarization of an AGN.Comparison of our models to polarization observations of large AGN samplesgreatly favors geometrically compact clumpy tori over extended ones.

Modeling optical and UV polarization of AGNs III. From uniform-density to clumpy regions