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Based on our previous modeling of AGN feedback in isolated ellipticalgalaxies (Gan et al. 2014) using the MACER (Massive AGN Controlled EllipticalsResolved) code, we extend and improve the model to include rotation, to limitstar formation to regions of high density and low temperature, to facilitateangular momentum transfer via the Toomre instability in gaseous disks, and toimprove the treatment of hot mode (low accretion rate) AGN feedback. The modelgalaxy now has an extended dark matter profile that matches with standardobservations, but has a resolution of parsecs in the inner region and resolvesthe Bondi radius. We find that the results agree reasonably well with a panoplyof observations: (1) both AGN activity and star formation are primarily incentral cold gaseous disks, are bursty and mainly driven by the Toomreinstability; (2)AGN duty cycle agrees well with the Soltan argument, i.e., theAGN spends most of its lifetime when it is in low luminosity (half of time with$L/L_{Edd}<7\times10^{-5}$), while emitting most of its energy when it is inhigh luminosity (half of radiant energy emitted with $L/L_{Edd}>0.06$); (3) thetotal star formation is $\sim$ few percents of the initial stellar mass,occurring in the bursts that would be associated with the observed E+Aphenomenon. Most of the star formation occurs in the circumnuclear disk of asize <1 kpc, which is in agreement with recent observations; (4) the ISM X-rayluminosity varies within a reasonable range (median $L_{\rm X,ISM}=9.1\times10^{39}$ erg/s) in agreement with observations.

MACER improved: AGN feedback computed in rotating early-type galaxies at high resolution