Confirming NGC 6231 as the parent cluster of the runaway high-mass X-ray binary HD 153919/4U 1700-37 with Gaia DR2

Abstract

Context. A significant fraction (10-20%) of the most massive stars move through space with a high (v 30 km s −1 ) velocity. One of the possible physical explanations is that a supernova in a compact binary system results in a high recoil velocity of the system. If the system remains bound, it can be subsequently observed as a spectroscopic binary (SB1), a high-mass X-ray binary, a compact binary, and finally a gravitational-wave event.Aims. If such a system is traced back to its parent cluster, binary evolution models can be tested in great detail. Methods. The Gaia proper motions and parallaxes are used to demonstrate that the high-mass X-ray binary HD 153919/4U 1700-37 originates from NGC 6231, the nucleus of the OB association Sco OB1.Results. The O supergiant and its compact companion, of which the physical nature (a neutron star or a black hole) is unknown, move with a space velocity of 63 ± 5 km s −1 with respect to NGC 6231. The kinematical age of the system is 2.2 ± 0.1 Myr. The parallaxes and accurate proper motions in Gaia DR2 were used to perform a membership analysis of NGC 6231; 273 members are identified, of which 268 have good quality photometry. The distance to NGC 6231 is 1.63 ± 0.15 kpc. Isochrone fitting results in an age of 4.7 ± 0.4 Myr and an extinction A V to the cluster of 1.7 ± 0.1. With the identification of NGC 6231 as the parent cluster, the upper limit on the age of the progenitor of 4U1700-37 at the moment of the supernova explosion is 3.0 ± 0.5 Myr. Conclusions. With these constraints, the evolutionary history of the system can be reconstructed with an initial mass of the progenitor of the compact object > 60 M . The high mass, the extreme mass ratio, and short orbital separation of the system make it difficult to produce possible progenitor systems through population synthesis. We propose that the system experienced a Case A mass transfer phase before the supernova, which typically widens a binary. In order to create a progenitor system that does not merge, a lot of angular momentum must be lost from the system during the phase of mass transfer and/or an asymmetry in the supernova explosion provides a kick resulting in the observed orbital parameters. Given its current high space velocity and the derived evolutionary history, the compact object in the system is more likely to have received a large natal kick, which suggests that it is more likely a neutron star than a black hole. HD153919/4U1700-37 might be a prototype in the Milky Way for the progenitor of gravitational wave events such as GW190412.

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

“…In this context, it is very interesting to identify the parent stellar group of HMXBs in the Galaxy (see, e.g., Ankay et al 2001;van der Meij et al 2021). Recently, the HMXB candidate 1H11255-567 (µ 1 and µ 2 Cru, spectral types B2+B5, together with a possible neutron star) was traced back to the Lower-Centaurus-Crux group, where it could have originated up to ∼ 1.8 Myr ago in a supernova at 89−112 pc (Neuhäuser et al 2020).…”