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Negative feedback from active galactic nuclei (AGN) is the leading mechanismfor the quenching of massive galaxies in the vast majority of modern galaxyevolution models. However, direct observational evidence that AGN feedbackcauses quenching on a population scale is lacking. Studies have shown thatluminous AGN are preferentially located in gas-rich and star-forming galaxies,an observation that has sometimes been suggested to be in tension with anegative AGN feedback picture. We investigate three of the current cosmologicalsimulations (IllustrisTNG, EAGLE and SIMBA) along with post-processed modelsfor molecular hydrogen gas masses and perform similar tests to those used byobservers. We find that the simulations predict: (i) no strong negative trendsbetween AGN luminosity and molecular gas fraction or sSFR; (ii) bothhigh-luminosity ($L_{bol}>10^{44}$ erg/s) and high-Eddington ratio (>1%) AGNare preferentially located in galaxies with high molecular gas fractions andsSFR; and (iii) that the gas-depleted and quenched fractions of AGN hostgalaxies are lower than a control sample of non-active galaxies. These threefindings are in qualitative agreement with observational samples at $z=0$ and$z=2$ and show that such results are not in tension with the presence of strongAGN feedback, which all simulations we employ require to produce realisticmassive galaxies. However, we also find quantifiable differences betweenpredictions from the simulations, which could allow us to observationally testthe different subgrid feedback models.

Cosmological simulations predict that AGN preferentially live in gas-rich, star-forming galaxies despite effective feedback