The origin of the high-mass X-ray binary 4U 2206+54/BD +53 2790

TL;DR

This study traces the origin and evolutionary history of the high-mass X-ray binary 4U 2206+54, revealing its likely formation in the Cepheus OB1 association and detailing the supernova event that created its neutron star.

Contribution

It provides the first kinematic analysis linking 4U 2206+54 to Cepheus OB1 and estimates the supernova kick velocity and progenitor mass.

Findings

System originated in Cepheus OB1 subgroup.

Progenitor lost 4-9 solar masses in supernova.

Neutron star received a kick velocity of 200-350 km/s.

Abstract

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$M_{\odot}$.