  The blazar OJ287 is the most promising (and the only) case for an
extragalactic binary black hole system inspiralling under the action of
gravitational radiation reaction. At present, though it is not possible to
directly observe the binary components, it is possible to observe the jet
emanating form the primary black hole. We argue that the orbital motion of the
secondary black hole is reflected in the wobble of the jet and demonstrate that
the wobble is orbital position dependent. The erratic wobble of the jet,
reported in Agudo et al. (2012), is analyzed by taking into account the binary
nature of the system and we find that the erratic component of jet wobble is
very small.
