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 \(2.{7}_{-0.3}^{+1.9}\,\times \,1{0}^{6}\) 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.

高速恒星和奇特的 G 天体围绕中心超大质量黑洞 （SMBH） 人马座 A* （Sgr A*） 运行。G 天体和高速恒星一起构成了 S 星团。与理论预测相反，尚未发现 Sgr A* 附近的双星系统。在这里，我们报告了在 S 星团中检测到一个光谱双星系统，其分量质量分别为 2.80 ± 0.50 M_⊙ 和 0.73 ± 0.14 M_⊙，假设采用边缘配置。根据视向速度的周期性变化，我们发现这两个分量的轨道周期为 372±3 天。由于次级的半长轴为 1.59±0.01 AU，远低于其约 42.4 AU 的潮汐破坏半径，因此双星系统对 Sgr A* 的破坏是稳定的。该系统被称为 D9，与 G 天体相似。我们估计 D9 的年龄为 \（2.{7}_{-0.3}^{+1.9}\，\times \，1{0}^{6}\） yr，这与 SMBH 诱导的 von Zeipel-Lidov-Kozai 周期期的时间尺度相当，约为 10⁶ 年，导致系统在不久的将来合并。因此，G 对象的填充可能由合并前的二进制文件和合并后的产物组成。D9 的探测意味着 S 星系团中的双星系统有可能在超大质量黑洞 Sgr A* 附近居住大约 10⁶ 年。