Searching for TeV Gamma-Ray Emission from SGR 1935+2154 during Its 2020 X-Ray and Radio Bursting Phase
Searching for TeV Gamma-Ray Emission from SGR 1935+2154 during Its 2020 X-Ray and Radio Bursting Phase
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DOI：
10.3847/1538-4357/ac0fe1
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发表时间：
2021-09
期刊：
影响因子：
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通讯作者：
H. Abdalla;F. Aharonian;F. Ait Benkhali;E. Angüner;C. Arcaro;C. Armand;T. Armstrong;H. Ashkar
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文献类型：
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作者：
H. Abdalla;F. Aharonian;F. Ait Benkhali;E. Angüner;C. Arcaro;C. Armand;T. Armstrong;H. Ashkar
磁性超频是快速无线电爆发（FRB）的最合理的解释 - 神秘的强大无线电脉冲，其持续时间为几毫秒，亮度温度高。这种情况的第一个观察证据是在2020年4月获得的，当时从银河磁盘的方向和软伽玛射线中继器SGR \，1935年+2154检测到FRB。在Swift卫星上的BAT仪器（H.E.S.S.）触发了后续观察，FRB在Swift Satellite上的蝙蝠仪器（H.E.S.S.）触发了后续观察，在FRB之前进行了两次伽马射线爆发警报。 H.E.S.S. 1935年4月28日，Sgr \ 1935+2154在2小时中观察到了2个小时。观察结果与积分和Fermi-GBM检测到的磁盘的X射线突发一致，因此提供了第一个非常高的能量（VHE）Gamma-ray观测值。在这些后续观察过程中获得的高质量数据使我们能够对短期瞬变进行搜索。在Energies上没有明显的信号$ e> 0.6 $ 〜TEV，并且得出了持久和瞬态发射的上限。我们在这里介绍了这些观察结果的分析，并讨论了H.E.S.S.的结果和前景。软伽玛射线中继器的后续计划。
Magnetar hyperflares are the most plausible explanation for fast radio bursts (FRB) -- enigmatic powerful radio pulses with durations of several milliseconds and high brightness temperatures. The first observational evidence for this scenario was obtained in 2020 April when a FRB was detected from the direction of the Galactic magnetar and soft gamma-ray repeater SGR\,1935+2154. The FRB was preceded by two gamma-ray outburst alerts by the BAT instrument aboard the Swift satellite, which triggered follow-up observations by the High Energy Stereoscopic System (H.E.S.S.). H.E.S.S. has observed SGR\,1935+2154 for 2 hr on 2020 April 28. The observations are coincident with X-ray bursts from the magnetar detected by INTEGRAL and Fermi-GBM, thus providing the first very high energy (VHE) gamma-ray observations of a magnetar in a flaring state. High-quality data acquired during these follow-up observations allow us to perform a search for short-time transients. No significant signal at energies $E>0.6$~TeV is found and upper limits on the persistent and transient emission are derived. We here present the analysis of these observations and discuss the obtained results and prospects of the H.E.S.S. follow-up program for soft gamma-ray repeaters.