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Using the two large cosmological hydrodynamical simulations, Horizon-AGN(H-AGN) and Horizon-noAGN (H-noAGN, no AGN feedback), we investigate how atypical sub-grid model for AGN feedback affects the evolution of the totaldensity profiles (dark matter + stars) at the effective radius of massiveearly-type galaxies (M*>10^11 Msun). We have studied the dependencies of themass-weighted density slope gamma'_tot with the effective radius, the galaxymass and the host halo mass at z~0.3 and found that the inclusion of AGNfeedbackalways leads to a much better agreement with observational values andtrends. Our analysis suggests also that the inclusion of AGN feedback favours astrong correlation between gamma'_tot and the density slope of the dark mattercomponent while, in the absence of AGN activity, gamma'_tot is rather stronglycorrelated with the density slope of the stellar component. Finally, we findthat gamma'_tot derived from our samples of galaxies increases from z=2 toz=0,in good agreement with the expected observational trend. The derived slopesare slightly lower than in the data when AGN is included because the simulatedgalaxies tend to be too extended, especially the least massive ones. However,the simulated compact galaxies without AGN feedback have gamma'_tot values thatare significantly too high compared to observations.

Total density profile of massive early-type galaxies in Horizon-AGN simulation: impact of AGN feedback and comparison with observations