  We report the discovery of a probable CH star in the core of the Galactic
globular cluster M14, identified from an integrated-light spectrum of the
cluster obtained with the MOS spectrograph on the CFHT. From a high- resolution
echelle spectrum of the same star obtained with the Hydra fiber positioner and
bench spectrograph on the WIYN telescope, we measure a radial velocity of
$-53.0\pm1.2$ km s$^{-1}$. Although this velocity is inconsistent with
published estimates of the systemic radial velocity of M14 (eg, ${\bar {v_r}}
\approx -123$ km s$^{-1}$), we use high-precision Hydra velocities for 20 stars
in the central 2.6 arcminutes of M14 to calculate improved values for the
cluster mean velocity and one-dimensional velocity dispersion: $-59.5\pm1.9$ km
s$^{-1}$ and $8.2\pm1.4$ km s$^{-1}$, respectively. Both the star's location
near the tip of the red giant branch in the cluster color magnitude diagram and
its radial velocity therefore argue for membership in M14. Since the
intermediate-resolution MOS spectrum shows not only enhanced CH absorption but
also strong Swan bands of C$_2$, M14 joins Omega Cen as the only globular
clusters known to contain classical CH stars. Although evidence for its
duplicity must await additional radial velocity measurements, the CH star in
M14 is probably, like all field CH stars, a spectroscopic binary with a
degenerate (white dwarf) secondary. The candidate and confirmed CH stars in M14
and Omega Cen, and in a number of Galactic dSph galaxies, may then owe their
existence to the long timescales for the shrinking and coalescence of hard
binaries in low-concentration environments.
