  Based on the Gaia EDR3 astrometric parameters and our new systemic radial
velocity of the high-mass X-ray binary 4U 2206+54/BD+53 2790, we studied the
trace back motion of the system and propose that it originated in the subgroup
of the Cepheus OB1 association (Age~4-10 Myr) with its brightest star BD+53
2820 (B0V; L~$10^{4.7}$L$_\odot$). The kinematic age of 4U 2206+54 is about
2.8$\pm$0.4 Myr, it is at a distance of 3.1-3.3 kpc and has a space velocity of
75-100 km/s with respect to this member star (BD+53 2820) of the Cep OB1
association. This runaway velocity indicates that the progenitor of the neutron
star hosted by 4U 2206+54 lost about 4-9 $M_{\odot}$ during the supernova
explosion and the latter one received a kick velocity of at least 200-350 km/s.
Since the high-mass X-ray binary 4U 2206+54/BD+53 2790 was born as a member of
a subgroup of Cep OB1, the initially most massive star in the system terminated
its evolution within ~7-9 Myr, corresponding to an initial mass >=
32$M_{\odot}$.
