HXMT identification of a non-thermal X-ray burst from SGR J1935+2154 and with FRB 200428

Li, C. K.; Lin, L.; Xiong, S. L.; Ge, M. Y.; Li, X. B.; Li, T. P.; Lu, Fangjun; Zhang, S. N.; Tuo, Y. L.; Nang, Y.; Zhang, B.; Xiao, Shuo; Chen, Y.; Song, L. M.; Xu, Y. P.; Liu, C. Z.; Jia, S.; Cao, X. L.; Qu, J. L.; Zhang, S.; Gu, Y. D.; Liao, J. Y.; Zhao, Xiaofan; Tan, Ying; Nie, J. Y.; Zhao, H. S.; Zheng, S.; Zheng, Y. G.; Luo, Q.; Cai, C.; Li, B.; Xue, W. C.; Bu, Q. C.; Chang, Zhi; Chen, G.; Chen, L.; Chen, T. X.; Chen, Y. B.; Chen, Y. P.; Cui, Weiwei; Deng, J. K.; Dong, Yanting; Du, Yongzhai; Fu, M. X.; Gao, G. H.; Gao, He; Gao, Min; Guan, J.; Guo, Chengcheng; Han, Danxiang; Huang, Y.; Jia, Haiqiang; Jiang, Luhua; Jiang, Weichun; Jin, J.; Jin, Yongjie; Kong, L. D.; Li, G.; Li, M. S.; Li, W.; Li, X.; Li, Xiaofeng; Li, Y. G.; Li, Z. W.; Liang, X. H.; Liu, B. S.; Liu, G. Q.; Liu, Han–Wen; Liu, X. J.; Liu, Y. N.; Lü, Bo; Lu, X. F.; Luo, T.; Ma, Xiang; Meng, Bin; Ou, G.; Sai, N.; Shang, R. C.; Song, X. Y.; Sun, Liang; Tao, Lian; Wang, C.; Wang, G. F.; Wang, J.; Wang, W. S.; Wang, Y. S.; Wen, Xiang-Yang; Wu, B. B.; Wu, Mei‐Hwan; Xiao, G. C.; Xu, He; Yang, Jiawei; Yang, S.; Yang, Yi-Jung; Yi, Q. B.; Yin, Q. Q.; You, Y.; Zhang, A. M.; Zhang, C. M.; Zhang, Faming; Zhang, H. M.; Zhang, J.; Zhang, T.; Zhang, W.; Zhang, W. C.; Zhang, W. Z.; Zhang, Y.; Zhang, Y. J.; Zhang, Zhaojian; Zhang, Zhi; Zhang, Z. L.; Zhou, D. K.; Zhou, Jianfeng; Zhu, Yajun; Zhuang, R. L.

doi:10.1038/s41550-021-01302-6

Cited by 182 publications

(143 citation statements)

References 36 publications

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“…The local nature makes measurements of the object and its environment much easier and with much greater detail. In fact, a linkage between the production of soft gamma bursts in this source and FRBs is naturally suggested: the same two events as the FRBs, with the appropriate delay due to dispersion by interstellar electrons, were detected by γray instruments [24][25][26][27][28] (though some authors suggest that different source types may be responsible for these vs extragalactic FRBs [29]).…”

Section: Application To Sgr1935 + 2154mentioning

confidence: 99%

Distinguishing time clustering of astrophysical bursts

2021

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Many astrophysical bursts can recur, and their time series structure or pattern could be closely tied to the emission and system physics. While analysis of periodic events is well established, some sources, e.g., some fast radio bursts and soft gamma-ray emitters, are suspected of more subtle and less explored periodic windowed behavior: the bursts themselves are not periodic, but the activity only occurs during periodic windows. We focus here on distinguishing periodic windowed behavior from merely clustered events through time clustering analysis, using techniques analogous to spatial clustering, demonstrating methods for identifying and characterizing the behavior. An important aspect is accounting for the "curious incident of the dog in the night time"-lack of bursts carries information. As a worked example, we analyze six years of data from the soft gamma repeater SGR1935 þ 2154, deriving a window period of 231 days and 55% duty cycle.

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Section: Application To Sgr1935 + 2154mentioning

confidence: 99%

Distinguishing time clustering of astrophysical bursts

2021

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“…Assuming the same spectral parameters as observed in the FRB 200428associated X-ray burst (ref. 6 ), the 1 s 3σ upper limit of the energy flux in the 8-200 keV band from Fermi/GBM data is 8.1 × 10 −8 erg cm −2 s −1 , and the upper limits from GECAM and Insight-HXMT data are 4.2 × 10 −8 erg cm −2 s −1 (15-200 keV) and 1.8 × 10 −8 erg cm −2 s −1 (200-3000 keV), respectively. Accordingly, the ratio between the luminosity in radio and γ-ray bands, L radio /L γ , is constrained at ≥ 1.4 × 10 −7 (8-200 keV), and ≥ 6.3 × 10 −7 (200-3000 keV).…”

Section: Simultaneous High-energy Observationsmentioning

confidence: 99%

“…Fast radio bursts (FRBs) are highly dispersed radio bursts prevailing in the universe [1][2][3] . The recent detection of FRB 200428 from a Galactic magnetar [4][5][6][7][8] suggested that at least some FRBs originate from magnetars, but it is unclear whether the majority of cosmological FRBs, especially the actively repeating ones, are produced from the magnetar channel. Here we report the detection of 1863 polarised bursts from the repeating source FRB 20201124A 9 during a dedicated radio observational campaign of Five-hundred-meter Aperture Spherical radio Telescope (FAST).…”

mentioning

confidence: 99%

A fast radio burst source at a complex magnetised site in a barred galaxy

Xu¹,

Niu²,

Chen³

et al. 2021

Preprint

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Fast radio bursts (FRBs) are highly dispersed radio bursts prevailing in the universe. The recent detection of FRB~200428 from a Galactic magnetar suggested that at least some FRBs originate from magnetars, but it is unclear whether the majority of cosmological FRBs, especially the actively repeating ones, are produced from the magnetar channel. Here we report the detection of 1863 polarised bursts from the repeating source FRB~20201124A during a dedicated radio observational campaign of Five-hundred-meter Aperture Spherical radio Telescope (FAST). The large sample of radio bursts detected in 88 hr over 54 days indicate a significant, irregular, short-time variation of the Faraday rotation measure (RM) of the source during the first 36 days, followed by a constant RM during the later 18 days. Significant circular polarisation up to 75\% was observed in a good fraction of bursts. Evidence suggests that some low-level circular polarisation originates from the conversion from linear polarisation during the propagation of the radio waves, but an intrinsic radiation mechanism is required to produce the higher degree of circular polarisation. All of these features provide evidence for a more complicated, dynamically evolving, magnetised immediate environment around this FRB source. Its host galaxy was previously known. Our optical observations reveal that it is a Milky-Way-sized, metal-rich, barred-spiral galaxy at redshift z=0.09795+-0.00003, with the FRB residing in a low stellar density, interarm region at an intermediate galactocentric distance, an environment not directly expected for a young magnetar formed during an extreme explosion of a massive star.

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“…It is also shown that the X-ray bursts overlapping the double-peaked CHIME radio burst have an unusually hard spectrum, and it is suggested that these X-rays and the radio bursts arise from a common scenario [15]. Furthermore, the non-thermal nature of the Insight-HXMT burst [19] points to the production of multi-TeV electrons. Multi-GeV to TeV gamma-ray emission via the inverse-Compton process may then accompany this X-ray emission.…”

Section: Introductionmentioning

confidence: 99%

Observation of burst activity from SGR1935+2154 associated to first galactic FRB with H.E.S.S.

Kostunin¹,

Abdalla²,

Aharonian³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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Fast radio bursts (FRB) are enigmatic powerful single radio pulses with durations of several milliseconds and high brightness temperatures suggesting coherent emission mechanism. For the time being a number of extragalactic FRBs have been detected in the high-frequency radio band including repeating ones. The most plausible explanation for these phenomena is magnetar hyperflares. The first observational evidence of this scenario was obtained in April 2020 when an FRB was detected from the direction of the Galactic magnetar and soft gamma repeater SGR1935+2154. The FRB was preceded with a number of soft gamma-ray bursts observed by Swift-BAT satellite, which triggered the follow-up program of the H.E.S.S. imaging atmospheric Cherenkov telescopes (IACTs). H.E.S.S. has observed SGR1935+2154 over a 2 hour window few hours prior to the FRB detection by STARE2 and CHIME. The observations overlapped with other X-ray bursts from the magnetar detected by INTEGRAL and Swift-BAT, thus providing first observations of a magnetar in a flaring state in the very-high energy domain. We present the analysis of these observations, discuss the obtained results and prospects of the H.E.S.S. follow-up program for soft gamma repeaters and anomalous X-ray pulsars.

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HXMT identification of a non-thermal X-ray burst from SGR J1935+2154 and with FRB 200428

Cited by 182 publications

References 36 publications

Distinguishing time clustering of astrophysical bursts

Distinguishing time clustering of astrophysical bursts

A fast radio burst source at a complex magnetised site in a barred galaxy

Observation of burst activity from SGR1935+2154 associated to first galactic FRB with H.E.S.S.

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