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The requirement of intermediate line component in the recently observedspectra of several AGNs points to possibility of the existence of a physicallyseparate region between broad line region (BLR) and narrow line region (NLR).In this paper we explore the emission from intermediate line region (ILR) byusing the photoionization simulations of the gas clouds distributed radiallyfrom the AGN center. The gas clouds span distances typical for BLR, ILR andNLR, and the appearance of dust at the sublimation radius is fully taken intoaccount in our model. Single cloud structure is calculated under the assumptionof the constant pressure. We show that the slope of the power law cloud densityradial profile does not affect the existence of ILR in major types of AGN. Wefound that the low ionization iron line, Fe~II, appears to be highly sensitivefor the presence of dust and therefore becomes potential tracer of dust contentin line emitting regions. We show that the use of disk-like cloud densityprofile computed at the upper part of the accretion disc atmosphere reproducesthe observed properties of the line emissivities. In particular, the distanceof H${\beta}$ line inferred from our model agrees with that obtained from thereverberation mapping studies in Sy1 galaxy NGC 5548.

Intermediate-line Emission in AGNs: The Effect of Prescription of the Gas Density