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We examine the connection between the properties of the circumgalactic medium(CGM) and the quenching and morphological evolution of central galaxies in theEAGLE and IllustrisTNG simulations. The simulations yield very different medianCGM mass fractions, $f_{\rm CGM}$, as a function of halo mass, $M_{200}$, withlow-mass haloes being significantly more gas-rich in IllustrisTNG than inEAGLE. Nonetheless, in both cases scatter in $f_{\rm CGM}$ at fixed $M_{200}$is strongly correlated with the specific star formation rate and the kinematicmorphology of central galaxies. The correlations are strongest for $\simL^\star$ galaxies, corresponding to the mass scale at which AGN feedbackbecomes efficient. This feedback elevates the CGM cooling time, preventing gasfrom accreting onto the galaxy to fuel star formation, and thus establishing apreference for quenched, spheroidal galaxies to be hosted by haloes with low$f_{\rm CGM}$ for their mass. In both simulations, $f_{\rm CGM}$ correlatesnegatively with the host halo's intrinsic concentration, and hence with itsbinding energy and formation redshift, primarily because early halo formationfosters the rapid early growth of the central black hole (BH). This leads to alower $f_{\rm CGM}$ at fixed $M_{200}$ in EAGLE because the BH reaches highaccretion rates sooner, whilst in IllustrisTNG it occurs because the central BHreaches the mass threshold at which AGN feedback is assumed to switch fromthermal to kinetic injection earlier. Despite these differences, there isconsensus from these state-of-the-art simulations that the expulsion ofefficiently-cooling gas from the CGM is a crucial step in the quenching andmorphological evolution of central galaxies.

The quenching and morphological evolution of central galaxies is facilitated by the feedback-driven expulsion of circumgalactic gas