Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023
The transient Galactic black hole candidate Swift J1727.8-1613 went through an outburst for the very first time in 2023 August and lasted for almost 6 months. We study the timing and spectral properties of this source using publicly available archival Insight-HXMT data for the first 10 observation I...
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2024-01-01
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| author | Kaushik Chatterjee Santanu Mondal Chandra B. Singh Mutsumi Sugizaki |
| author_facet | Kaushik Chatterjee Santanu Mondal Chandra B. Singh Mutsumi Sugizaki |
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| description | The transient Galactic black hole candidate Swift J1727.8-1613 went through an outburst for the very first time in 2023 August and lasted for almost 6 months. We study the timing and spectral properties of this source using publicly available archival Insight-HXMT data for the first 10 observation IDs that last from MJD 60181 to 60198 with a total of 92 exposures for each of the three energy bands. We have detected quasi-periodic oscillations (QPOs) in a frequency range of 0.21 ± 0.01–1.86 ± 0.01 Hz by fitting the power density spectrum. Based on the model-fitted parameters and properties of the QPOs, we classify them as type C in nature. We also conclude that the origin of the QPOs could be the shock instabilities in the transonic advective accretion flows around black holes. The spectral analysis was performed using simultaneous data from the three onboard instruments LE, ME, and HE of Insight-HXMT in the broad energy band of 2−150 keV. To achieve the best fit, spectral fitting required a combination of models, e.g., interstellar absorption, power-law, multicolor disk–blackbody continuum, Gaussian emission/absorption, and reflection by neutral material. From the spectral properties, we found that the source was in an intermediate state at the start of the analysis period and was transitioning to the softer states. The inner edge of the accretion disk moved inward in progressive days following the spectral nature. We found that the source has a high inclination of 78°−86°. The hydrogen column density from the model fitting varied in the range of (0.12 ± 0.02−0.39 ± 0.08) × 10 ^22 cm ^−2 . |
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| spelling | doaj-art-63570f6feda44f89bd3148e8aa8615b22025-08-20T02:39:04ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01977214810.3847/1538-4357/ad8dc4Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023Kaushik Chatterjee0https://orcid.org/0000-0002-6252-3750Santanu Mondal1https://orcid.org/0000-0003-0793-6066Chandra B. Singh2https://orcid.org/0000-0002-7782-5719Mutsumi Sugizaki3https://orcid.org/0000-0002-1190-0720South-Western Institue For Astronomy Research, Yunnan University , University Town, Chenggong, Kunming 650500, People's Republic of China ; kaushik@ynu.edu.cn, mails.kc.physics@gmail.comIndian Institute of Astrophysics , II Block Koramangala, Bengaluru 560034, Karnataka, India ;South-Western Institue For Astronomy Research, Yunnan University , University Town, Chenggong, Kunming 650500, People's Republic of China ; kaushik@ynu.edu.cn, mails.kc.physics@gmail.comNational Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing 100012, People's Republic of China; Kanazawa University , Kakumamachi, Kanazawa, Ishikawa 9201192, JapanThe transient Galactic black hole candidate Swift J1727.8-1613 went through an outburst for the very first time in 2023 August and lasted for almost 6 months. We study the timing and spectral properties of this source using publicly available archival Insight-HXMT data for the first 10 observation IDs that last from MJD 60181 to 60198 with a total of 92 exposures for each of the three energy bands. We have detected quasi-periodic oscillations (QPOs) in a frequency range of 0.21 ± 0.01–1.86 ± 0.01 Hz by fitting the power density spectrum. Based on the model-fitted parameters and properties of the QPOs, we classify them as type C in nature. We also conclude that the origin of the QPOs could be the shock instabilities in the transonic advective accretion flows around black holes. The spectral analysis was performed using simultaneous data from the three onboard instruments LE, ME, and HE of Insight-HXMT in the broad energy band of 2−150 keV. To achieve the best fit, spectral fitting required a combination of models, e.g., interstellar absorption, power-law, multicolor disk–blackbody continuum, Gaussian emission/absorption, and reflection by neutral material. From the spectral properties, we found that the source was in an intermediate state at the start of the analysis period and was transitioning to the softer states. The inner edge of the accretion disk moved inward in progressive days following the spectral nature. We found that the source has a high inclination of 78°−86°. The hydrogen column density from the model fitting varied in the range of (0.12 ± 0.02−0.39 ± 0.08) × 10 ^22 cm ^−2 .https://doi.org/10.3847/1538-4357/ad8dc4X-ray binary starsBlack holesStellar accretion disksShocksCompact radiation sources |
| spellingShingle | Kaushik Chatterjee Santanu Mondal Chandra B. Singh Mutsumi Sugizaki Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023 The Astrophysical Journal X-ray binary stars Black holes Stellar accretion disks Shocks Compact radiation sources |
| title | Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023 |
| title_full | Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023 |
| title_fullStr | Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023 |
| title_full_unstemmed | Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023 |
| title_short | Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023 |
| title_sort | insight hxmt view of the black hole candidate swift j1727 8 1613 during its outburst in 2023 |
| topic | X-ray binary stars Black holes Stellar accretion disks Shocks Compact radiation sources |
| url | https://doi.org/10.3847/1538-4357/ad8dc4 |
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