  The final aim of this paper is to expand the sparse group of X-ray binaries
with gamma-ray counterparts as laboratories to study high-energy processes
under physical conditions that periodically repeat. A follow-up of a candidate
system has been carried out. We applied both photometric and spectroscopic
techniques in the optical domain together with a period analysis using the
phase dispersion minimization and CLEAN methods. A tentative period search was
also conducted in the gamma-ray domain. Our main result is having established
the binary nature of the optical star and X-ray emitter HD 3191 towards the
Fermi gamma-ray source 4FGL J0035.8+6131, the last one proposed to be
associated with a blazar of an unknown type. An orbital period close to 16 days
is reported for HD 3191 together with a likely rotation, or pulsation, period
of about 0.6 d. Although no convincing evidence for the orbital cycle has been
found in the Fermi light curve up to now, the confirmed presence of a high-mass
X-ray binary towards 4FGL J0035.8+6131 now strengthens the need for caution
about its true nature.
