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In this paper we investigate the role of AGN feedback on the late stageevolution of elliptical galaxies by performing high-resolution hydrodynamicalsimulation in the {\it MACER} framework. By comparing models that take intoaccount different feedback mechanisms, namely AGN and stellar feedback, we findthat AGN feedback is crucial in keeping the black hole in a low accretion stateand suppressing the star formation. We then compare the energy from AGNradiation and wind deposited in the galaxy and find that only wind cancompensate for the radiative cooling of the gas in the galaxy. Further, weinvestigate which plays the dominant role, the wind from the cold (quasar) orhot (radio) feedback modes, by examining the cumulative energy output andimpact area to which the wind can heat the interstellar medium and suppressstar formation. Our results indicate that first, although AGN spends most ofits time in hot (radio) mode, the cumulative energy output is dominated by theoutburst of the cold mode. Second, only the impact area of the cold-mode windis large enough to heat the gas in the halo, while the hot-mode wind is not.Additionally, the cold-mode wind is capable of sweeping up the material fromstellar mass loss. These results indicate the dominant role of cold-mode wind.The limitations of our model, including the absence of jet feedback, arediscussed.

On the dominant role of wind in the quasar feedback mode in the late stage evolution of massive elliptical galaxies