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...
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Nature Portfolio
2024-12-01
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| Series: | Nature Communications |
| Online Access: | https://doi.org/10.1038/s41467-024-54748-3 |
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| author | Florian Peißker Michal Zajaček Lucas Labadie Emma Bordier Andreas Eckart Maria Melamed Vladimír Karas |
| author_facet | Florian Peißker Michal Zajaček Lucas Labadie Emma Bordier Andreas Eckart Maria Melamed Vladimír Karas |
| author_sort | Florian Peißker |
| collection | DOAJ |
| description | 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. |
| format | Article |
| id | doaj-art-37f5e8a738cf47a7a7eb463b8430a09e |
| institution | DOAJ |
| issn | 2041-1723 |
| language | English |
| publishDate | 2024-12-01 |
| publisher | Nature Portfolio |
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| series | Nature Communications |
| spelling | doaj-art-37f5e8a738cf47a7a7eb463b8430a09e2025-08-20T02:39:41ZengNature PortfolioNature Communications2041-17232024-12-0115111110.1038/s41467-024-54748-3A binary system in the S cluster close to the supermassive black hole Sagittarius A*Florian Peißker0Michal Zajaček1Lucas Labadie2Emma Bordier3Andreas Eckart4Maria Melamed5Vladimír Karas61.Physikalisches Institut, Universität zu Köln1.Physikalisches Institut, Universität zu Köln1.Physikalisches Institut, Universität zu Köln1.Physikalisches Institut, Universität zu Köln1.Physikalisches Institut, Universität zu Köln1.Physikalisches Institut, Universität zu KölnAstronomical Institute, Czech Academy of SciencesAbstract 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.https://doi.org/10.1038/s41467-024-54748-3 |
| spellingShingle | Florian Peißker Michal Zajaček Lucas Labadie Emma Bordier Andreas Eckart Maria Melamed Vladimír Karas A binary system in the S cluster close to the supermassive black hole Sagittarius A* Nature Communications |
| title | A binary system in the S cluster close to the supermassive black hole Sagittarius A* |
| title_full | A binary system in the S cluster close to the supermassive black hole Sagittarius A* |
| title_fullStr | A binary system in the S cluster close to the supermassive black hole Sagittarius A* |
| title_full_unstemmed | A binary system in the S cluster close to the supermassive black hole Sagittarius A* |
| title_short | A binary system in the S cluster close to the supermassive black hole Sagittarius A* |
| title_sort | binary system in the s cluster close to the supermassive black hole sagittarius a |
| url | https://doi.org/10.1038/s41467-024-54748-3 |
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