Impact of the Galactic Disk and Large Magellanic Cloud on the
  Trajectories of Hypervelocity Stars Ejected from the Galactic Center
  We consider how the gravity of the Galactic disk and the Large Magellanic
Cloud (LMC) modifies the radial motions of hypervelocity stars (HVSs) ejected
from the Galactic Center. For typical HVSs ejected towards low (high) Galactic
latitudes, the disk bends trajectories by up to 30 degrees (3-10 deg). For many
lines-of-sight through the Galaxy, the LMC produces similar and sometimes
larger deflections. Bound HVSs suffer larger deflections than unbound HVSs.
Gravitational focusing by the LMC also generates a factor of two overdensity
along the line-of-sight towards the LMC. With large enough samples,
observations can detect the non-radial orbits and the overdensity of HVSs
towards the LMC. For any Galactic potential model, the Galactic rest-frame
tangential velocity provides an excellent way to detect unbound and nearly
bound HVSs within 10 kpc of the Sun. Similarly, the rest-frame radial velocity
isolates unbound HVSs beyond 10-15 kpc from the Sun. Among samples of unbound
HVSs, measurements of the radial and tangential velocity serve to distinguish
Galactic Center ejections from other types of high velocity stars.
