  We present binary galaxy merger simulations with varying mass ratios and
different progenitor morphologies. The simulations include mergers of gas-rich
disks (Sp-Sp), of early-type galaxies and disks (E-Sp, mixed mergers), and
mergers of early-type galaxies (E-E, dry mergers). We follow the dynamics of
gas, stars and dark matter, and include radiative cooling, star formation and
black hole (BH) accretion. For Sp-Sp mergers, the peak star formation rate and
BH accretion rate decrease and the growth timescales of the central black holes
and newly formed stars increase with higher progenitor mass ratios. The peak BH
accretion rate typically occurs shortly after the time of BH merging for low
progenitor mass ratios (e.g. 3:1 and lower), whereas for higher progenitor mass
ratios there is no clear correlation between the peak BH accretion rate and BH
merging time. The termination of star formation by BH feedback in disk mergers
is significantly less important for higher progenitor mass ratios (e.g. 3:1 and
higher). In addition, the inclusion of BH feedback suppresses efficiently star
formation in dry E-E mergers and mixed E-Sp mergers. All merger remnants,
independent of their progenitors, follow the observed relations between the
central BH mass and the stellar velocity dispersion M_BH-sigma, the bulge mass
M_BH-M_* and the bulge binding energy M_BH-M_{*}sigma^2, with the dominant
source of scatter arising from variations in the initial gas mass fraction. The
normalizations for all relations and the simulated slope of the M_BH-sigma and
M_BH-M_{*}sigma^2 relations are in good agreement with the observations,
whereas the simulated slope of the M_BH-M_* relation is slightly steeper
compared to the observations. (abridged)
