  There is mounting evidence for the coevolution of galaxies and their embedded
massive black holes (MBHs) in a hierarchical structure formation paradigm. To
tackle the nonlinear processes of galaxy-MBH interaction, we describe a
self-consistent numerical framework which incorporates both galaxies and MBHs.
The high-resolution adaptive mesh refinement (AMR) code Enzo is modified to
model the formation and feedback of molecular clouds at their characteristic
scale of 15.2 pc and the accretion of gas onto a MBH. Two major channels of MBH
feedback, radiative feedback (X-ray photons followed through full 3D adaptive
ray tracing) and mechanical feedback (bipolar jets resolved in high-resolution
AMR), are employed. We investigate the coevolution of a 9.2e11 Msun galactic
halo and its 1e5 Msun embedded MBH at redshift 3 in a cosmological LCDM
simulation. The MBH feedback heats the surrounding ISM up to 1e6 K through
photoionization and Compton heating and locally suppresses star formation in
the galactic inner core. The feedback considerably changes the stellar
distribution there. This new channel of feedback from a slowly growing MBH is
particularly interesting because it is only locally dominant, and does not
require the heating of gas globally on the disk. The MBH also self-regulates
its growth by keeping the surrounding ISM hot for an extended period of time.
