  Two decades on, the study of hypervelocity stars is still in its infancy.
These stars can provide novel constraints on the total mass of the Galaxy and
its Dark Matter distribution. However how these stars are accelerated to such
high velocities is unclear. Various proposed production mechanisms for these
stars can be distinguished using chemo-dynamic tagging. The advent of Gaia and
other large surveys have provided hundreds of candidate hyper velocity objects
to target for ground based high resolution follow-up observations. We conduct
high resolution spectroscopic follow-up observations of 16 candidate late-type
hyper velocity stars using the Apache Point Observatory and the McDonald
Observatory. We derive atmospheric parameters and chemical abundances for these
stars. We measure up to 22 elements, including the following nucleosynthetic
families: {\alpha} (Mg, Si, Ca, Ti), light/Odd-Z (Na, Al, V, Cu, Sc), Fe-peak
(Fe, Cr, Mn, Co, Ni, Zn), and Neutron Capture (Sr, Y, Zr, Ba, La, Nd, Eu). Our
kinematic analysis shows one candidate is unbound, two are marginally bound,
and the remainder are bound to the Galaxy. Finally, for the three unbound or
marginally bound stars, we perform orbit integration to locate possible
globular cluster or dwarf galaxy progenitors. We do not find any likely
candidate systems for these stars and conclude that the unbound stars are
likely from the the stellar halo, in agreement with the chemical results. The
remaining bound stars are all chemically consistent with the stellar halo as
well.
