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We present the wavelength-resolved reverberation mapping (RM) of combinedMgII and UV FeII broad-line emissions for two intermediate redshifts(z$\sim$1), luminous quasars - HE 0413-4031 and HE 0435-4312, monitored by theSALT and 1-m class telescopes between 2012-2022. Through this technique, we aimto disentangle the Mg II and FeII emission regions and to build aradius-luminosity relation for UV FeII emission, which has so far remainedunconstrained. Several methodologies have been applied to constrain the timedelays for total MgII and FeII emissions. In addition, this technique isperformed to quantify the inflow or outflow of broad-line region gas around thesupermassive black hole and to disentangle the emission/emitting regions fromlines produced in proximity to each other. The mean total FeII time delay isnearly equal to the mean total Mg II time delay for HE 0435-4312 suggesting aco-spatiality of their emissions. However, in HE 0413-4031, the mean FeII timedelay is found to be longer than the mean MgII time delay, suggesting that FeIIis produced at longer distances from the black hole. The UV Fe II R-L relationis updated with these two quasars and compared with the optical FeII relation,which suggests that the optical FeII region is located further than the UV FeIIby a factor of 1.7-1.9 i.e. $R_{\rm FeII-opt}\sim(1.7-1.9)R_{\rm FeII-UV}$. Wedetected a weak pattern in the time delay vs. wavelength relation, suggestingthat the MgII broad-line originates a bit closer to the SMBH than the UV FeII,however, the difference is not very significant. Comparison of MgII, UV, andoptical FeII R-L relations suggests that the difference may be larger forlower-luminosity sources, possibly with the MgII emission originating furtherfrom the SMBH. In the future, more RM data will be acquired to put betterconstraints on these trends, in particular the UV FeII R-L relation.

astronomy and astrophysics

Wavelength-resolved reverberation mapping of intermediate redshift  quasars HE 0413-4031 and HE 0435-4312: Dissecting Mg II, optical Fe II, and  UV Fe II emission regions