  Hot subdwarf stars with F-K main sequence binary companions have been known
for decades, but the first orbital periods for such systems were published just
recently. Current observations suggest that most have long periods, on the
order of years, and that some are or once were hierarchical triple systems. As
part of a survey with the Hobby-Eberly Telescope, we have been monitoring the
radial velocities of several composite-spectra binaries since 2005 in order to
determine their periods, velocities, and eccentricities. Here we present
observations and orbital solutions for two of these systems, PG 1449+653 and PG
1701+359. Similar to the other sdB+F/G/K binaries with solved orbits, their
periods are long, 909 d and 734 d, respectively, and pose a challenge to
current binary population synthesis models of hot subdwarf stars. Intrigued by
their relatively large systemic velocities, we also present a kinematical
analysis of both targets and find that neither is likely a member of the
Galactic thin disk.
