  The three objects have been identified as members of the recently recognized
class of Gamma Doradus stars, which exhibit multi-periodic photometric
variations that are thought to arise from non-radial pulsation. The particular
objects treated here also prove to be spectroscopic binaries, for which we
provide reliable orbits. The radial velocities exhibit unusually large
residuals, in which some of the photometric periodicities can be traced. Some
of the same periodicities are also demonstrated by the observed variations in
the line profiles, which are quantified here simply in terms of the
line-widths.
