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We append two additional black hole (BH) accretion models, namely viscousdisc and gravitational torque-driven accretion, into the NumericalInvestigation of a Hundred Astrophysical Objects (NIHAO) project of galaxysimulations. We show that these accretion models, characterized by a weakerdependence on the BH mass compared to the commonly used Bondi-Hoyle accretion,naturally create a common evolutionary track (co-existence) between the mass ofthe BH and the stellar mass of the galaxy, even without any direct coupling viafeedback (FB). While FB is indeed required to control the final BH and stellarmass of the galaxies, our results suggest that FB might not be the leadingdriver of the cosmic co-evolution between these two quantities; in thesemodels, co-evolution is simply determined by the shared central gas supply.Conversely, simulations using Bondi-Hoyle accretion show a two-step evolution,with an early growth of stellar mass followed by exponential growth of thecentral supermassive black hole (SMBH). Our results show that the modelling ofBH accretion (sometimes overlooked) is an extremely important part of BHevolution and can improve our understanding of how scaling relations emerge andevolve, and whether SMBH and stellar mass co-exist or co-evolve through cosmictime.

Co-Evolution vs. Co-existence: The Effect of Accretion Modelling on the Evolution of Black Holes and Host Galaxies