A binary system in the S cluster close to the supermassive black hole Sagittarius A*

Abstract

High-velocity stars and peculiar G objects orbit the central supermassive black hole (SMBH) Sagittarius A* (Sgr A*). Together, the G objects and high-velocity stars constitute the S cluster. In contrast with theoretical predictions, no binary system near Sgr A* has been identified. Here, we report the detection of a spectroscopic binary system in the S cluster with the masses of the components of 2.80 $\pm$ 0.50 M$_{\odot}$ and 0.73 $\pm$ 0.14 M$_{\odot}$, assuming an edge-on configuration. Based on periodic changes in the radial velocity, we find an orbital period of 372 $\pm$ 3 days for the two components. The binary system is stable against the disruption by Sgr A* due to the semi-major axis of the secondary being 1.59 $\pm$ 0.01 AU, which is well below its tidal disruption radius of approximately 42.4 AU. The system, known as D9, shows similarities to the G objects. We estimate an age for D9 of 2.7$^{+1.9}_{-0.3}$ x 10$^6$ yr that is comparable to the timescale of the SMBH-induced von Zeipel-Lidov-Kozai cycle period of about 10$^6$ yr, causing the system to merge in the near future. Consequently, the population of G objects may consist of pre-merger binaries and post-merger products. The detection of D9 implies that binary systems in the S cluster have the potential to reside in the vicinity of the supermassive black hole Sgr A* for approximately 10$^6$ years.