  Spectral energy distribution (SED) fitting is one of most commonly used
techniques to study the dust properties in Active Galactic Nuclei (AGN). Works
implementing this technique commonly use radiative transfer models that assume
a variety of dust properties. Despite the key role of this aspect, limited
effort has been put forward to explore the chemical composition, the role of
different optical properties, and the grain size distribution of dust, all of
which can have a substantial impact on the theoretical radiative transfer
calculations. In this work, we explore the role of the dust chemical
composition in the AGN dusty torus through SED fitting to \emph{Spitzer}/IRS
spectra of a sample of 49 nearby AGN with silicate features in emission. We
implement a mineralogy model including the popular astronomical silicates and a
set of oxides and amorphous silicates with different grain sizes. We find that
best fits use principally porous alumina, periclase, and olivine. In terms of
mass fractions, $\sim99\%$ of the dust is composed of dust grains of size
$\rm{0.1 \mu m}$, with a $<1\%$ contribution from $\rm{3 \mu m}$ grains.
Moreover, the astronomical silicates have a very low occurrence in the best
fits, suggesting that they are not the most suited dust species to reproduce
the silicate features in our sample.
