MACER Improved: AGN Feedback Computed in Rotating Early-type Galaxies at High Resolution

Based on our previous modeling of active galactic nucleus (AGN) feedback in isolated elliptical galaxies using the MACER (Massive AGN Controlled Ellipticals Resolved) code, we extend and improve the model to include rotation, to facilitate angular momentum transfer via the Toomre instability in gaseous disks, to limit the star formation to regions of high density and low temperature, 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 it 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 are mainly driven by the Toomre instability. (2) The 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 the time with L/L Edd < 7 × 10 -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 roughly a few percent 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 a circumnuclear disk of size ≤1 kpc, which is in agreement with recent observations. (4) The interstellar medium X-ray luminosity varies within a reasonable range (median L X,ISM = 9.1 × 10 39 erg s -1 ), in agreement with observations.