  We present limits on the ejection of old-population HVS from a sample of over
290,000 stars selected from the SDSS. We derive the speed at the solar circle
from the measured positions and radial velocities by assuming a radial orbit
and adopting a simple isothermal model of the Galactic halo, which enables us
to identify candidate bound and unbound ejectees. We find 4 candidate bound
F-stars from this sample, all with negative Galactocentric radial velocity
(i.e., returning toward the GC). We additionally find 2 candidate unbound stars
(one F and one G), however, existing proper motion measurements make these
unlikely to be emerging from the GC. These data place an upper limit on the
rate of ejection of old-population stars from the GC of ~45/Myr. Comparing to
the rate for more massive B-star ejectees of ~0.5/Myr, our limit on the rate of
ejection of old-population HVS shows that the mass function at the GC is not
bottom-heavy and is consistent with being normal. Future targeted surveys of
old-population HVS could determine if it is indeed top-heavy.
