  We used the CLUMPY torus models and a Bayesian approach to fit the infrared
spectral energy distributions (SEDs) and ground-based high-angular resolution
mid-infrared spectroscopy of 13 nearby Seyfert galaxies. This allowed us to put
tight constraints on torus model parameters such as the viewing angle, the
radial thickness of the torus Y, the angular size of the cloud distribution
sigma_torus, and the average number of clouds along radial equatorial rays N_0.
The viewing angle is not the only parameter controlling the classification of a
galaxy into a type 1 or a type 2. In principle type 2s could be viewed at any
viewing angle as long as there is one cloud along the line of sight. A more
relevant quantity for clumpy media is the probability for an AGN photon to
escape unabsorbed. In our sample, type 1s have relatively high escape
probabilities, while in type 2s, as expected, tend to be low. Our fits also
confirmed that the tori of Seyfert galaxies are compact with torus model radii
in the range 1-6pc. The scaling of the models to the data also provided the AGN
bolometric luminosities, which were found to be in good agreement with
estimates from the literature. When we combined our sample of Seyfert galaxies
with a sample of PG quasars from the literature to span a range of
L_bol(AGN)~10^{43}-10^{47}erg/s, we found plausible evidence of the receding
torus. That is, there is a tendency for the torus geometrical covering factor
to be lower at high AGN luminosities than at low AGN luminosities. This is
because at low AGN luminosities the tori appear to have wider angular sizes and
more clouds along radial equatorial rays. We cannot, however rule out the
possibility that this is due to contamination by extended dust structures not
associated with the dusty torus at low AGN luminosities, since most of these in
our sample are hosted in highly inclined galaxies. (Abridged)
