Fig. 13.
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Schematic representation of MgII and FeII emission regions derived from the total time delays in both quasars and comparison with CTS C30.10 (Prince et al. 2022). We also noticed that, in CTS C30.10, the MgII time delay is shorter than the FeII time delay, which suggests a higher inclination of the source, leading to the invisibility of the MgII emission coming from the other side of the black hole.
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