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By using high-resolution 1D hydrodynamical simulations, we investigate theeffects of purely mechanical feedback from super massive black holes (SMBHs) inthe evolution of elliptical galaxies for a broad range of feedback efficienciesand compare the results to four major observational constraints. In particular,we focus on 1) the central black hole to stellar mass ratio of the host galaxy,2) the lifetime of the luminous quasar phase, 3) the mass of stars formed inthe host galaxy within the last Gyr, and 4) the X-ray luminosity of the hotdiffuse gas. As a result, we try to pin down the most successful range ofmechanical feedback efficiencies. We find that while low feedback efficienciesresult in too much growth of the SMBH, high efficiencies totally blow out thehot interstellar gas, and the models are characterized by very low thermalX-ray luminosity well below the observed range. The net lifetime of the quasarphase is strongly coupled to the mass ratio between SMBH and its host galaxy,while the X-ray luminosity is generally correlated to the recent star formationwithin the last Gyr. When considering the popularly adopted model of theconstant feedback efficiency, the feedback energy deposited into the ambientmedium should be more than 0.01% of the SMBH accretion energy to be consistentwith the SMBH mass to stellar mass ratio in the local universe. Yet, the X-rayluminosity of the hot gas favors about 0.005% of the accretion energy as themechanical AGN feedback energy. We conclude that the purely mechanical feedbackmode is unlikely to be simultaneously compatible with all four observabletests, even allowing a broad range of feedback efficiencies, and that includingboth radiative and mechanical feedback together may be a solution to comply theobservational constraints. [abridged]

Feedback from central black holes in elliptical galaxies. II: Can purely mechanical energy feedback models work?