tokens: between the two models, though the BHWR model has a slightly higher duty cycle than the onyWind model that matches the correspondingly higher SMBH mass growth (compare Fig. 3 ). Figure 5. Time distribution of different accretion rates in units of the Eddington limit (so-called BH duty cycles) for the different models (see legend) compared to observations (square: Ho 2009 , circles: Greene Ho 2007 , upward-pointing triangles: Kauffmann Heckman 2009 , downward-pointing triangles: Heckman etal. 2004 , all taken from Novak etal. 2011 ). Both simulated models fall above all of the observed values at Eddington ratios of 1 and 10percent. 4 BH-GOVERNED ISM EVOLUTION IN THE GALACTIC CENTRE In the previous section, we have shown that feedback from the central SMBH is both necessary to, and capable of keeping an isolated ETG quiescent. The more physically complete feedback model, including both wind and radiative feedback, is more efficient at this than the pure wind-feedback model. In this section and the next, we will now examine how the feedback achieves the quiescence through its influence on the galactic gas, and how it creates metal-rich, large-scale outflows that enrich the CGM. We begin with Fig. 6 , which shows colour maps of the surface density (top row) and the density-weighted average temperature (central row) in a 10kpc thick, 10 10kpc wide region around the galactic centre (and therefore around the central SMBH), as well as the temperaturedensity phase diagrams of all the galactic gas (bottom row). In the maps, the line of sight is chosen to be parallel to the initial angular momentum of the hot halo. The solid vertical and horizontal lines in the phase diagrams mark the star formation thresholds in density and temperature, respectively, i.e. gas in the bottom-right corner of the diagrams is star forming. The individual temperaturedensity bins are colour-coded for gas particle number density, which is rising from blue to red colours. The dashed line marks the resolution of the simulation limit following the Jeans mass criterion. Above the dashed line, the Jeans mass of the gas is resolved, i.e. it is larger than the kernel mass M ker N ngb m gas 10 7 M , while it is unresolved below the line, meaning that gas in this region could collapse under self-gravity due to numerical noise. Almost all of the gas particles with unresolved Jeans mass are in the star-forming region of the phase space, and will be turned into star particles if they stay in this region. Hence, while this resolution does not allow us to make predictions about the substructure of the dense, cool gas, it is high enough to investigate the global and larger scale effects of AGN feedback that interest us in this paper. The three left columns show the state of the three models (from left to right: no-BH, BH-W, BH-WR) at the end of the simulation time, while the last column to the right shows the state of the BH-WR model about 30Myr before the end of the simulation. Figure 6. Maps
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