  Hypervelocity stars (HVS) traverse the Galaxy from the central black hole to
the outer halo. We show that the Galactic potential within 200 pc acts as a
high pass filter preventing low velocity HVS from reaching the halo. To trace
the orbits of HVS throughout the Galaxy, we construct two forms of the
potential which reasonably represent the observations in the range 5--100,000
pc, a simple spherically symmetric model and a bulge-disk-halo model. We use
the Hills mechanism (disruption of binaries by the tidal field of the central
black hole) to inject HVS into the Galaxy and compute the observable spatial
and velocity distributions of HVS with masses in the range 0.6--4 Msun. These
distributions reflect the mass function in the Galactic Center, properties of
binaries in the Galactic Center, and aspects of stellar evolution and the
injection mechanism. For 0.6--4 Msun main sequence stars, the fraction of
unbound HVS and the asymmetry of the velocity distribution for their bound
counterparts increases with stellar mass. The density profiles for unbound HVS
decline with distance from the Galactic Center approximately as r^{-2} (but are
steeper for the most massive stars which evolve off the main sequence during
their travel time from the Galactic Center); the density profiles for the bound
ejecta decline with distance approximately as r^{-3}. In a survey with a
limiting visual magnitude V of 23, the detectability of HVS (unbound or bound)
increases with stellar mass.
