Projected (2D) density profiles of all nine models. Red lines represent adiabatic SMBH growth models after T = 8 Gyr (Models 1–8) and T = 6.7 Gyr (Model 9), whereas black lines show reference models without growing SMBHs (i.e., ΔM_• = 0). The density slopes, γ, are fitted within half the size of the initial break radii by using a simple power-law approximation. Hence, they are influenced by the outer profile and we quote them with their sign. In ascending order of the computed reference Models 1–9 these are: γ_ref = −0.26; −0.26; −0.3; −0.3; −0.28; −0.23; −0.25; −0.3; −0.3. The quantity Δγ = γ_ref − γ_adiab ≥ 0 results from a growing density cusp due to adiabatic SMBH growth. Evidently, accretion rates with lead to a cusp regeneration process. Smaller accretion rates (Models 1–5) have no strong impact on the innermost 2D density slope. In panel 9 a pure Sersic n = 4 model is added for comparison (black dotted line). The solid blue line corresponds to the nbody6 computation of the same model. It is in excellent agreement with the solid red line. The red dashed line is similar, but is scaled to a 1.5 times larger host galaxy mass, similar to the Phoenix BCG (McDonald et al. 2013).