Schematic view of the anisotropy in the radiation between the observer and the BLR cloud. Our model considers a simple shrinking of the radial position of the BLR to match the reverberation-mapped R_BLR estimate, by filtering the incoming radiation from the accretion disc. Therefore, the net SED seen by the BLR differs from the SED seen by a distant observer. This illustration applies to I Zw 1-like sources, i.e. Type-1 Narrow-line Seyfert galaxies with high Fe II emission, which are the context of this study.