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

Florian Peißker (), Michal Zajaček, Lucas Labadie, Emma Bordier, Andreas Eckart, Maria Melamed and Vladimír Karas
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Florian Peißker: Universität zu Köln
Michal Zajaček: Universität zu Köln
Lucas Labadie: Universität zu Köln
Emma Bordier: Universität zu Köln
Andreas Eckart: Universität zu Köln
Maria Melamed: Universität zu Köln
Vladimír Karas: Czech Academy of Sciences

Nature Communications, 2024, vol. 15, issue 1, 1-11

Abstract: 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 ± 0.50 M⊙ and 0.73 ± 0.14 M⊙, assuming an edge-on configuration. Based on periodic changes in the radial velocity, we find an orbital period of 372±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±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 $$2.{7}_{-0.3}^{+1.9}\,\times \,1{0}^{6}$$ 2 . 7 − 0.3 + 1.9 × 1 0 6 yr that is comparable to the timescale of the SMBH-induced von Zeipel-Lidov-Kozai cycle period of about 106 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 106 years.

Date: 2024
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DOI: 10.1038/s41467-024-54748-3

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