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We carry out a comparative analysis of the relation between the mass ofsupermassive black holes (BHs) and the stellar mass of their host galaxies at$0.2<z<1.7$ using well-matched observations and multiple state-of-the-artsimulations (e.g., Massive Black II, Horizon-AGN, Illustris, TNG and asemi-analytic model). The observed sample consists of 646 uniformly-selectedSDSS quasars ($0.2 < z < 0.8$) and 32 broad-line active galactic nuclei (AGNs;$1.2<z<1.7$) with imaging from Hyper Suprime-Cam (HSC) for the former andHubble Space Telescope (HST) for the latter. We first add realisticobservational uncertainties to the simulation data and then construct asimulated sample in the same manner as the observations. Over the full redshiftrange, our analysis demonstrates that all simulations predict a level ofintrinsic scatter of the scaling relations comparable to the observations whichappear to agree with the dispersion of the local relation. Regarding the meanrelation, Horizon-AGN and TNG are in closest agreement with the observations atlow and high redshift ($z\sim$ 0.2 and 1.5, respectively) while the othersimulations show subtle differences within the uncertainties. For insight intothe physics involved, the scatter of the scaling relation, seen in the SAM, isreduced by a factor of two and closer to the observations after adopting a newfeedback model that considers the geometry of the AGN outflow. The consistencyin the dispersion with redshift in our analysis supports the importance of bothquasar- and radio-mode feedback prescriptions in the simulations. Finally, wehighlight the importance of increasing the sensitivity (e.g., using the JamesWebb Space Telescope), thereby pushing to lower masses and minimizing biasesdue to selection effects.

Concordance between observations and simulations in the evolution of the mass relation between supermassive black holes and their host galaxies