Modeling the Strongest Silicate Emission Features of Local Type 1 AGNs

We measure the 10 and 18 mu m silicate features in a sample of 67 local (z.<.0.1) type 1 active galactic nuclei (AGN) with available Spitzer spectra dominated by nonstellar processes. We find that the 10 mu m silicate feature peaks at 10.3(-0.9)(+0.7) mu m with a strength (Si-p = ln f(p)(spectrum)/f(p)(continuum)) of 0.11+(+0.15)(-0.36), while the 18 mu m one peaks at 17.3(-0.7)(+0.4) mu m with a strength of 0.14(-0.06)(+0.06). We select from this sample sources with the strongest 10 mu m silicate strength (sigma(Si10) mu m > 0.28, 10 objects). We carry out a detailed modeling of the infrared spectrometer/Spitzer spectra by comparing several models that assume different geometries and dust composition: a smooth torus model, two clumpy torus models, a two-phase medium torus model, and a disk+outflow clumpy model. We find that the silicate features are well modeled by the clumpy model of Nenkova et al., and among all models, those including outflows and complex dust composition are the best. We note that even in AGN-dominated galaxies, it is usually necessary to add stellar contributions to reproduce the emission at the shortest wavelengths.