Schematic representation of the Mg II and Fe II emission regions. The mean distance of the Mg II and Fe II region from the BH is ∼0.23 pc, estimated from the rest frame time delays, 276 days and 270 days for Mg II and Fe II, respectively. The Fe II emission also exhibits a shorter time delay in the rest frame, 180 days, which indicates the larger extent of the Fe II region with respect to the Mg II emission region in the direction away from the SMBH. Hence, due to a non-negligible inclination of the observer, the reprocessed emission from the Fe II region finally tends to come to the observer sooner. The secondary time delays at ∼570 and ∼680 days can potentially be attributed to the mirror-effect, i.e., the Mg II and Fe II emission, respectively, coming to the observer from the other side of the accretion disc, which is supported by the temporal difference of (570 − 270) = 300 days, which corresponds to ∼0.25 pc, i.e., one additional disk crossing of photons. However, the Fe II emission coming from the more distant part across the disk is partially shielded by the Mg II line-emitting region closer in with respect to the observer. Color does not represent the density of the cloud.