  In this paper we explore the intermediate line region (ILR) by using the
photoionisation simulations of the gas clouds present at different radial
distances from the center, corresponding to the locations from BLR out to NLR
in four types of AGNs. We let for the presence of dust whenever conditions
allow for dust existence. All spectral shapes are taken from the recent
multi-wavelength campaigns. The cloud density decreases with distance as a
power law. We found that the slope of the power law density profile does not
affect the line emissivity radial profiles of major emission lines: H${\beta}$,
He~II, Mg~II, C~III] ~and [O~III]. When the density of the cloud at the
sublimation radius is as high as 10$^{11.5}$ cm$^{-3}$, the ILR should clearly
be seen in the observations independently of the shape of the illuminating
radiation. Moreover, our result is valid for low ionization nuclear emission
regions of active galaxies.
