The origin of the high-mass X-ray binary 4U 2206+54/BD+532790

Based on the Gaia EDR3 astrometric parameters and our new systemic radial velocity of the high-mass X-ray binary 4U 2206+54/BD+532790, we studied the trace back motion of the system and propose that it originated in the subgroup of the Cepheus OB1 association (Age similar to 4-10 Myr) with its brightest star, BD+532820 (B0V; L similar to 10(4.7) L-circle dot). The kinematic age of 4U 2206+54 is about 2.8 +/- 0.4 Myr, it is at a distance of 3.1-3.3 kpc and has a space velocity of 75-100 km s(-1) with respect to this member star (BD+532820) 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-circle dot during the supernova explosion and the latter one received a kick velocity of at least 200-350 km s(-1) . Since the high-mass X-ray binary 4U 2206+54/BD+532790 was born as a member of a subgroup of Cep OB1, the initially most massive star in the system terminated its evolution within less than or similar to 7-9 Myr, corresponding to an initial mass greater than or similar to 32 M-circle dot.

Automated summary

Based on the astrometric parameters and radial velocity data, it is proposed that the high-mass X-ray binary 4U 2206+54/BD+532790 originated from a subgroup of the Cepheus OB1 association and its most massive star may have ended its evolution within approximately 7-9 million years.