  The star Cyg OB2 No. 9 is a well-known non-thermal radio emitter. Recent
theoretical work suggests that all such O-stars should be in a binary or a
multiple system. However, there is no spectroscopic evidence of a binary
component. Re-analysis of radio observations from the VLA of this system over
25 years has revealed that the non-thermal emission varies with a period of
2.35+-0.02 yr. This is interpreted as a strong suggestion of a binary system,
with the non-thermal emission arising in a wind-collision region. We derived
some preliminary orbital parameters for this putative binary and revised the
mass-loss rate of the primary star downward from previous estimates.
