  Repeated radial velocities have been measured for a sample of 10 subgiant CH
(sgCH) stars over a period of about 15 years. Long-term velocity variations are
exhibited by all but one star, and spectroscopic orbits have been calculated
for six of them. The periods are long, ranging from 876 to 4144 days. The
distribution of eccentricities and mass functions for sgCH star orbits are
similar to those for giant barium and CH stars, exhibiting significant orbital
dissipation relative to normal late-type binaries. It is concluded that all
sgCH stars are binaries, and like the barium and CH stars, they have had mass
transferred from a former asymptotic giant-branch star.
