Variation in stellar mass (M_⋆) of the host galaxies with their corresponding SFRs. Overplotted solid lines are analytical galaxy MS relations from Schreiber et al. (2015), at different redshifts with corresponding 1-σ uncertainty contours. We note that the highest redshift of our sample is z ∼ 1.8 (see Fig. 1), and thus the z = 3 trend lies outside our sample’s redshift range. The majority of the sources in our sample lie at a significant distance from the galaxy MS and tend to follow the high-redshift (z = 3) trend. In Fig. 9, we have colour-coded our sources with redshifts. Top left panel: For entire RL non-HBL, HBL and AstroSat-observed sources. Top right panel: For entire RQ non-HBL, HBL and AstroSat-observed sources. Bottom left panel: For RL non-HBL, HBL and AstroSat-observed sources that follow the criteria of Mountrichas et al. (2021). Bottom left panel: For RQ non-HBL, HBL and AstroSat-observed sources that follow the criteria of Mountrichas et al. (2021). The observed bimodality in the MS for RL quasars is evident. See Fig. 10 and discussions in Sect. 4.