  Close binary interactions may play a critical role in the formation of the
rapidly rotating Be stars. Mass transfer can result in a mass gainer star spun
up by the accretion of mass and angular momentum, while the mass donor is
stripped of its envelope to form a hot and faint helium star. FUV spectroscopy
has led to the detection of about 20 such binary Be+sdO systems. Here we report
on a three-year program of high quality spectroscopy designed to determine the
orbital periods and physical properties of five Be binary systems. These
binaries are long orbital period systems with $P =$ 95 to 237 days and with
small semi-amplitude $K_1<11$ km s$^{-1}$. We combined the Be star velocities
with prior sdO measurements to obtain mass ratios. A Doppler tomography
algorithm shows the presence of the He II $\lambda 4686$ line in the faint
spectrum of the hot companion in four of the targets. We discuss the observed
line variability and show evidence of phased-locked variations in the emission
profiles of HD 157832, suggesting a possible disk spiral density wave due to
the presence of the companion star. The stripped companions in HD 113120 and HD
137387 may have a mass larger than the 1.4 $M_\odot$ indicating that they could
be progenitors of Type Ib and Ic supernovae.
