  Using simulations of non-rotating supernova progenitors, we explore the kicks
imparted to and the spins induced in the compact objects birthed in core
collapse. We find that the recoil due to neutrino emissions can be a factor
affecting core recoil, comparable to and at times larger than the corresponding
kick due to matter recoil. This result would necessitate a revision of the
general model of the origin of pulsar proper motions. In addition, we find that
the sign of the net neutrino momentum can be opposite to the sign of the
corresponding matter recoil. As a result, at times the pulsar recoil and ejecta
can be in the same direction. Moreover, our results suggest that the duration
of the dipole in the neutrino emissions can be shorter than the duration of the
radiation of the neutron-star binding energy. This allows a larger dipole
asymmetry to arise, but for a shorter time, resulting in kicks in the observed
pulsar range. Furthermore, we find that the spin induced by the aspherical
accretion of matter can leave the residues of collapse with spin periods
comparable to those inferred for radio pulsars and that there seems to be a
slight anti-correlation between the direction of the induced spin and the net
kick direction. This could explain such a correlation among observed radio
pulsars. Finally, we find that the kicks imparted to black holes are due to the
neutrino recoil alone, resulting in birth kicks $\le$100 km s$^{-1}$ most of
the time.
