  How massive stars end their lives depends on the core mass, core angular
momentum, and hydrogen envelopes at death. However, these key physical facets
of stellar evolution can be severely affected by binary interactions. In turn,
the effectiveness of binary interactions itself varies greatly depending on the
initial conditions of the binaries, making the situation much more complex. We
investigate systematically how binary interactions influence core-collapse
progenitors and their fates. Binary evolution simulations are performed to
survey the parameter space of supernova progenitors in solar metallicity binary
systems and to delineate major evolutionary paths. We first study fixed binary
mass ratios ($q=M_2/M_1$ = 0.5, 0.7, and 0.9) to elucidate the impacts of
initial mass and initial separation on the outcomes, treating separately Type
Ibc supernova, Type II supernova, accretion induced collapse (AIC), rapidly
rotating supernova (RSN), black hole formation, and gamma ray burst (GRB). We
then conduct Binary Population Synthesis calculations for 12 models, varying
the initial parameter distributions and binary evolution parameters, to
estimate various supernova fractions. We obtain a Milky Way supernova rate
$R_{\rm SN} = (1.14$--$1.57) \times10^{-2} \, {\rm yr}^{-1}$ which is
consistent with observations. We find the rates of AIC, RSN, and GRB to be
$\sim 1/100$ the rate of regular supernovae. Our estimated GRB rates are higher
than the observed long GRB rate, but very close to the low luminosity GRB rate.
Furthering binary modeling and improving the inputs one by one will enable more
detailed studies of these and other transients associated with massive stars.
