  The binary status of gamma-Cas stars has been discussed while theoretically
examining the origin of their peculiar X-ray emission. However, except in two
cases, no systematic radial velocity monitoring of these stars had been
undertaken yet to clarify their status. We now fill this gap using TIGRE,
CARMENES, and UVES high-resolution spectroscopy. Velocities were determined for
16 stars, revealing shifts and/or changes in line profiles. The orbit of six
new binaries could be determined: the long periods (80-120d) and small velocity
amplitudes (5-7km/s) suggest low mass companions (0.6-1 M$_{\odot}$). The
properties of the known gamma-Cas binaries appear similar to those of other Be
systems, with no clear-cut separation between them. One of the new systems is a
candidate for a rare case of quadruple system involving a Be star. Five
additional gamma-Cas stars display velocity variations compatible with the
presence of companions, but no orbital solution could yet be formally
established for them hence they only receive the status of "binary candidate".
