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arXiv · 2201.07770

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

V. Hambaryan·K. A. Stoyanov·M. Mugrauer·R. Neuhäuser·W. Stenglein·R. Bischoff·K. -U. Michel·M. Geymeier·A. Kurtenkov·A. Kostov
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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$M_{\odot}$.

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V. Hambaryan, K. A. Stoyanov, M. Mugrauer, R. Neuhäuser, W. Stenglein, R. Bischoff, K. -U. Michel, M. Geymeier, A. Kurtenkov, A. Kostov. 2022-01-19. The origin of the high-mass X-ray binary 4U 2206+54/BD +53 2790. https://doi.org/10.1093/mnras%2Fstac184

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