MACER improved: AGN feedback computed in rotating early-type galaxies at
  high resolution
  Based on our previous modeling of AGN feedback in isolated elliptical
galaxies (Gan et al. 2014) using the MACER (Massive AGN Controlled Ellipticals
Resolved) code, we extend and improve the model to include rotation, to limit
star formation to regions of high density and low temperature, to facilitate
angular momentum transfer via the Toomre instability in gaseous disks, and to
improve the treatment of hot mode (low accretion rate) AGN feedback. The model
galaxy now has an extended dark matter profile that matches with standard
observations, but has a resolution of parsecs in the inner region and resolves
the Bondi radius. We find that the results agree reasonably well with a panoply
of observations: (1) both AGN activity and star formation are primarily in
central cold gaseous disks, are bursty and mainly driven by the Toomre
instability; (2)AGN duty cycle agrees well with the Soltan argument, i.e., the
AGN 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 in
high luminosity (half of radiant energy emitted with $L/L_{Edd}>0.06$); (3) the
total star formation is $\sim$ few percents of the initial stellar mass,
occurring in the bursts that would be associated with the observed E+A
phenomenon. Most of the star formation occurs in the circumnuclear disk of a
size <1 kpc, which is in agreement with recent observations; (4) the ISM X-ray
luminosity varies within a reasonable range (median $L_{\rm X,
ISM}=9.1\times10^{39}$ erg/s) in agreement with observations.
