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

Author

Y. J. Jin, Z. Chang, J. Y. Liao, H. M. Zhang, Y. F. Zhang, X. B. Li, Y. G. Li, Chun-sheng Zhang, Wenhan Jiang, Bo Li, Yu-Xuan Zhu, G. H. Gao, J. Jin, M. Wu, Y. Zhang, Xin-Fu Zhao, Zhi Zhang, Y. H. Tan, Y. X. Zhu, R. C. Shang, C. Cai, B. Lu, Fuqin Zhang, J. K. Deng, S. N. Zhang, W. C. Xue, X. X. Li, Y. G. Zheng, J. F. Zhou, Ming-Yu Ge, X. H. Ma, Wenxiong Li, Tian-Xiang Chen, F. J. Lu, Y. S. Wang, D. K. Zhou, Wei Cui, T. Zhang, Aimei Zhang, Lin Lin, Li-Ming Song, B. S. Liu, Lei Sun, C. Z. Liu, S. J. Zheng, Luhua Jiang, Y. P. Xu, B. B. Wu, X. L. Cao, Tao Luo, XiangYang Wen, Xue-Feng Lu, Bin Meng, S. Xiao, Y. B. Chen, Junqiang Zhang, Tong Li, H. W. Liu, N. Sai, Mao-Shun Li, Yunchao Liu, Sisi Yang, Y. J. Yang, S. M. Jia, Yuan You, L. D. Kong, Songbo Zhang, Cunguo Wang, Qi-Bin Yi, Yu-Dong Gu, Q. Q. Yin, Y. P. Chen, Xuelong Li, J. Guan, X. J. Liu, W. Z. Zhang, Yuan-Yuan Du, Gang Chen, X. H. Liang, G. C. Xiao, R. L. Zhuang, GuoQing Liu, Jia Huo, Y. Nang, Gang Li, Shaolin Xiong, Y. J. Zhang, H. Gao, Qiu-Yi Luo, Z. Zhang, Y. L. Tuo, J. W. Yang, Bing Zhang, B. Y. Wu, Lian Tao, X. Y. Song, H. S. Zhao, G. F. Wang, W. S. Wang, Ge Ou, W. C. Zhang, J. Y. Nie, Yi-Qiao Dong, Cheng-Cheng Guo, C. K. Li, H. Xu, Z. W. Li, Da-Wei Han, Z. L. Zhang, M. X. Fu, Yue Zhang, Ya Fang Huang, J. Z. Wang, L. Chen, Wan-Chang Zhang, Weiguang Cui, Qingcui Bu, Min Gao, and J. L. Qu

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Magnetar, 01 natural sciences, Coincidence, Radio spectrum, 0103 physical sciences, Thermal, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Event (particle physics), 0105 earth and related environmental sciences, Delay time
Abstract

Fast radio bursts (FRBs) are short pulses observed in radio band from cosmological distances. One class of models invoke soft gamma-ray repeaters (SGRs), or magnetars, as the sources of FRBs. Some radio pulses have been observed from some magnetars, however, no FRB-like events had been detected in association any magnetar burst, including one giant flare. Recently, a pair of FRB-like bursts (FRB 200428 hereafter) separated by milliseconds (ms) were detected from the general direction of the Galactic magnetar SGR J1935+2154. Here we report the detection of a non-thermal X-ray burst in the 1-250 keV energy band with the Insight-HXMT satellite, which we identify as emitted from SGR J1935+2154. The burst showed two hard peaks with a separation of 34 ms, broadly consistent with that of the two bursts in FRB 200428. The delay time between the double radio and X-ray peaks is about 8.57 s, fully consistent with the dispersion delay of FRB 200428. We thus identify the non-thermal X-ray burst is associated with FRB 200428 whose high energy counterpart is the two hard peaks in X-ray. Our results suggest that the non-thermal X-ray burst and FRB 200428 share the same physical origin in an explosive event from SGR J1935+2154., 24 pages, 9 figures, 6 tables; initial submission to a journal on May 9th, 2020. Significant changes include updated localization and detailed spectral evolution of the X-ray burst, and better determination of the two narrow X-ray peaks corresponding to the two radio pulses. Conclusions are strengthened. Nature Astronomy online on Feb. 18, 2021

Published
2021
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2. Insight-HXMT observations of jet-like corona in a black hole X-ray binary MAXI J1820+070

Author

Xiaobo Li, Zhu Liu, Y. L. Tuo, J. W. Yang, Shuang-Nan Zhang, Aimei Zhang, Yong Chen, Wei Wang, Li Chen, Mao-Shun Li, Hai-Sheng Zhao, C. K. Li, Cheng-Kui Li, Weimin Yuan, Yanji Yang, Juan Wang, Yu-Xuan Zhu, Ju Guan, Xiao-Fan Zhao, Bozena Czerny, Ling-Jun Wang, Qingwen Wu, Xufang Li, Gang Li, R. C. Shang, B. B. Wu, Shaolin Xiong, Yifei Zhang, Tong Zhang, X. Y. Song, Yongjie Zhang, N. Sai, Erlin Qiao, Yi Zhang, Ti-Pei Li, Lian Tao, Wei-Wei Cui, Wan-Chang Zhang, Bin Meng, Yue Zhu, Y. Nang, Liang Sun, Yu-Peng Chen, Ming-Yu Ge, Xiao-Jing Liu, Wei Cui, Zi-Gao Dai, Bobing Wu, Shu Zhang, Gang Chen, Bing Li, Yuan-Yuan Du, Zhi Chang, G. F. Wang, Xiang Ma, Ying Tan, L. D. Kong, T. Luo, Fangjun Lu, Guan-Hua Gao, Shuo Xiao, Juan Zhang, D. K. Zhou, Shu-Mei Jia, Y. P. Chen, Chichuan Jin, Bifang Liu, Wei Li, Jian-Feng Zhou, Ge Ou, Yupeng Xu, Bo Lu, Bei You, He Gao, Chen Wang, Fan Zhang, Yanguo Li, Chong Luo, Qi Luo, Jing Jin, Jing-Kang Deng, Li-Ming Song, Cheng-Cheng Guo, XiangYang Wen, Xiaohua Liang, C. X. Liu, C. Cai, Yue Huang, Yuan You, Jia Huo, Zi-Liang Zhang, J. C. Liu, Zhao Zhang, Yongwei Dong, Qi-Bin Yi, Mei Wu, W. C. Jiang, Jin-Yuan Liao, X. L. Cao, Xue-Feng Lu, Guang-Cheng Xiao, Wei Zhang, Chengmo Zhang, Yu-Dong Gu, Hong-Mei Zhang, Tian-Xiang Chen, GuoQing Liu, Y. N. Liu, Qian-Qing Yin, Zheng-Wei Li, Xian Li, Hongwei Liu, Sheng Yang, Wenshuai Wang, Luhua Jiang, Jin-Lu Qu, Jianyin Nie, Min-Xue Fu, Yu-Sa Wang, YongJie Jin, Yue Zhang, Qingcui Bu, Wen-Zhao Zhang, Da-Wei Han, M. Gao, and Shi-Jie Zheng

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Science, Phase (waves), X-ray binary, FOS: Physical sciences, General Physics and Astronomy, Astrophysics, Radiation, 01 natural sciences, Article, General Biochemistry, Genetics and Molecular Biology, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Jet (fluid), Multidisciplinary, Shock (fluid dynamics), 010308 nuclear & particles physics, General Chemistry, Corona, Astrophysics - Astrophysics of Galaxies, High-energy astrophysics, Black hole, Astrophysics of Galaxies (astro-ph.GA), Physics::Space Physics, Reflection (physics), Compact astrophysical objects, Astrophysics - High Energy Astrophysical Phenomena
Abstract

A black hole X-ray binary produces hard X-ray radiation from its corona and disk when the accreting matter heats up. During an outburst, the disk and corona co-evolves with each other. However, such an evolution is still unclear in both its geometry and dynamics. Here we report the unusual decrease of the reflection fraction in MAXI J1820+070, which is the ratio of the coronal intensity illuminating the disk to the coronal intensity reaching the observer, as the corona is observed to contrast during the decay phase. We postulate a jet-like corona model, in which the corona can be understood as a standing shock where the material flowing through. In this dynamical scenario, the decrease of the reflection fraction is a signature of the corona's bulk velocity. Our findings suggest that as the corona is observed to get closer to the black hole, the coronal material might be outflowing faster., 11 pages, 5 figures; published in Nature Communications; An artist's impression of Figure 5 is updated here, and the animation is available at http://youbei.work/research/

Published
2021

3. Quality assurance test and Failure Analysis of SiPM Arrays of GECAM Satellites

Author

Mao-Shun Li, C. Cai, X. Y. Zhao, J. Z. Wang, H. Z. Wang, Xu Zhou, Yuan-Yuan Du, C. Chen, Fan. Zhang, Z. Chang, F. Shi, Min Gao, Fangjun Lu, Fei Zhang, Z. H. An, Yupeng Xu, L. Li, D. J. Hou, G. Chen, Shaolin Xiong, Shuang-Nan Zhang, Yaqing Liu, XiangYang Wen, Bin Meng, X. L. Sun, Chengmo Zhang, J. J. He, S. Xiao, C. Y. Li, G. Li, H. Lu, Xian Li, Sheng Yang, D. L. Zhang, Xiaohua Liang, R. Gao, Ke Gong, J. W. Yang, X. Q. Li, Y. G. Li, C. Y. Zhang, Y. B. Xu, X. Y. Wen, Dongya Guo, Xiao-Jing Liu, Huanyu Wang, Y. S. Wang, and W. X. Peng

Subjects
Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, Computer science, business.industry, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Detector, Process (computing), FOS: Physical sciences, Instrumentation and Detectors (physics.ins-det), Reliability (semiconductor), Silicon photomultiplier, Nuclear Energy and Engineering, Electronic engineering, business, Aerospace, Quality assurance, Electrical impedance, Leakage (electronics)
Abstract

The Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) satellite consists of two small satellites. Each GECAM payload contains 25 gamma ray detectors (GRD) and 8 charged particle detectors (CPD). GRD is the main detector which can detect gamma-rays and particles and localize the Gamma-Ray Bursts (GRB),while CPD is used to help GRD to discriminate gamma-ray bursts and charged particle bursts. The GRD makes use of lanthanum bromide (LaBr3) crystal readout by SiPM. As the all available SiPM devices belong to commercial grade, quality assurance tests need to be performed in accordance with the aerospace specifications. In this paper, we present the results of quality assurance tests, especially a detailed mechanism analysis of failed devices during the development of GECAM. This paper also summarizes the application experience of commercial-grade SiPM devices in aerospace payloads, and provides suggestions for forthcoming SiPM space applications., Comment: 13 pages, 23 figures

Published
2021
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4. The design and performance of GRD onboard the GECAM satellite

Author

R. Gao, X. Q. Li, S. N. Zhang, C. Cai, C. Y. Zhang, Shaolin Xiong, Xilei Sun, W. X. Peng, F. J. Lu, Y. G. Li, J. Z. Wang, Cheng Chen, XiangYang Wen, Y. P. Xu, Xuelong Li, Mao-Shun Li, Y. S. Wang, H. J. Lu, J. J. He, X. Y. Wen, X. J. Liu, Yang Liu, Min Gao, H. Z. Wang, F. Shi, J. W. Yang, Bin Meng, Yuan-Yuan Du, Lei Li, Z. H. An, Chun-sheng Zhang, Xiaoran Zhao, D. Y. Guo, X. H. Liang, H. Wang, D. J. Hou, Fan Zhang, P. Y. Feng, S. Xiao, X. K. Zhou, K. Gong, G. Li, Z. Chang, Fei Zhang, Q. B. Yi, D. L. Zhang, Sisi Yang, C. Y. Li, G. F. Chen, Y. B. Xu, and Y. Zhao

Subjects
Nuclear and High Energy Physics, Computer science, Physics::Instrumentation and Detectors, Radioactive source, Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, Detector, Schematic, FOS: Physical sciences, Silicon photomultiplier, Nuclear Energy and Engineering, Electronic engineering, Satellite, Random vibration, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Energy (signal processing)
Abstract

Background: Each GECAM satellite payload contains 25 gamma-ray detectors (GRDs), which can detect gamma-rays and particles and can roughly localize the Gamma-Ray Bursts (GRBs). GRD was designed using lanthanum bromide (LaBr3) crystal as the sensitive material with the rear end coupled with silicon photomultiplier (SiPM) array for readout. Purpose: In aerospace engineering design of GRD, there are many key points to be studied. In this paper, we present the specific design scheme of GRD, the assembly and the performance test results of detectors. Methods: Based on Monte Carlo simulation and experimental test results, the specific schematic design and assembling process ofGRDwere optimized. After being fully assembled, theGRDswere conducted performance tests by using radioactive source and also conducted random vibration tests. Result and conclusion: The test results show that all satellite-borne GRDs have energy resolution, 10 pages, 15 figures

Published
2021
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5. Insight-HXMT observations of Swift J0243.6+6124: the evolution of RMS pulse fractions at super-Eddington luminosity

Author

Da-Wei Han, Luhua Jiang, Y. P. Xu, C. Cai, X. F. Li, Zhi Zhang, Mao-Shun Li, M. X. Fu, C. K. Li, Wenxiong Li, B. S. Liu, Wenhan Jiang, J. Z. Wang, X. H. Liang, Bing Li, Tao Luo, Y. B. Chen, B. Y. Wu, Weiguang Cui, S. Xiao, Qingcui Bu, Y. S. Wang, Z. W. Li, Chun-sheng Zhang, Yuan-Yuan Du, Xiaobo Li, X. L. Cao, J. Y. Nie, Y. X. Zhu, Ming-Yu Ge, Y. G. Zheng, Yi Jung Yang, J. Y. Liao, Min Gao, H. M. Zhang, Fuqin Zhang, S. N. Zhang, Y. Nang, Y. J. Jin, J. K. Deng, J. Guan, Wei Zhang, Z. Chang, Tian-Xiang Chen, Yi-Qiao Dong, Q. Q. Yin, Y. P. Chen, Cheng-Cheng Guo, Yunchao Liu, J. L. Qu, F. J. Lu, Long Ji, X. H. Ma, GuoQing Liu, Yan Ji Yang, Jia Huo, Gang Chen, W. C. Zhang, Y. F. Zhang, B. Lu, XiangYang Wen, B. B. Wu, Junqiang Zhang, Li-Ming Song, G Ou, Z. L. Zhang, Gang Li, Lian Tao, Y. H. Tan, D. K. Zhou, Xue-Feng Lu, Zhao Zhang, X. Y. Song, Ya Fang Huang, Tong Li, Lei Sun, L. Chen, Yuan You, J. F. Zhou, S. M. Jia, Yu-Xuan Zhu, Ling-Jun Wang, W. Z. Zhang, Qi-Bin Yi, Cunguo Wang, Wei Cui, T. Zhang, L. D. Kong, X. J. Liu, H. W. Liu, X. X. Li, Yu-Dong Gu, N. Sai, S. J. Zheng, Y. G. Li, Aimei Zhang, G. H. Gao, M. Wu, Y. Zhang, R. L. Zhuang, J. Jin, Xin-Fu Zhao, R. C. Shang, C. Z. Liu, Sisi Yang, Shaolin Xiong, Y. J. Zhang, H. Gao, Y. L. Tuo, J. W. Yang, Qiu-Yi Luo, G. C. Xiao, H. S. Zhao, Bin Meng, P. J. Wang, G. F. Wang, and W. S. Wang

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Swift, Physics, Astrophysics::High Energy Astrophysical Phenomena, Phase (waves), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Relative strength, Astrophysics::Cosmology and Extragalactic Astrophysics, Pulse (physics), Luminosity, symbols.namesake, Radiation pressure, Space and Planetary Science, Eddington luminosity, symbols, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, computer, Energy (signal processing), Astrophysics::Galaxy Astrophysics, computer.programming_language
Abstract

Based on Insight-HXMT data, we report on the pulse fraction evolution during the 2017–2018 outburst of the newly discovered first Galactic ultraluminous X-ray (ULX) source Swift J0243.6+6124. The pulse fractions of 19 observation pairs selected in the rising and fading phases with similar luminosity are investigated. The results show a general trend of the pulse fraction increasing with luminosity and energy at supercritical luminosity. However, the relative strength of the pulsation between each pair evolves strongly with luminosity. The pulse fraction in the rising phase is larger at luminosity below 7.71 × 1038 erg s−1, but smaller at above. A transition luminosity is found to be energy independent. Such a phenomenon is first confirmed by Insight-HXMT observations and we speculate that it may have relation with the radiation-pressure-dominated accretion disc.

Published
2020

6. Timing analysis of the black hole candidate EXO 1846-031 with Insight-HXMT monitoring

Author

Ju Guan, Yuan-Hang Zhang, Wei Zhang, Yue Zhang, W. C. Jiang, Y. G. Zheng, Cheng-Cheng Guo, Cheng-Kui Li, R. C. Shang, W. S. Wang, Shaolin Xiong, GuoQing Liu, Yongwei Dong, Tian-Xiang Chen, Yupeng Xu, Jian-Feng Zhou, Yu-Dong Gu, Qian-Qing Yin, Wei Li, Jianyin Nie, Wei Cui, X. L. Cao, Qingcui Bu, Yongjie Zhang, J. W. Yang, Jing-Yuan Liao, XiangYang Wen, Xiang Ma, Bing Li, Wen-Zhao Zhang, B. B. Wu, Tong Zhang, Zhao Zhang, Lian Tao, X. Y. Song, Zheng-Wei Li, Jing Jin, Zhi Chang, Mao-Shun Li, Yue Zhu, Jia Huo, Wei-Wei Cui, Xian Li, Hongwei Liu, Y. G. Li, Sheng Yang, Bo Lu, ShiJie Zheng, Jin-Lu Qu, H. W. Liu, Da-Wei Han, Wan-Chang Zhang, C. Cai, HongMei Zhang, Gang Li, Luhua Jiang, Yuan-Yuan Du, Min-Xue Fu, Yue Huang, He Xu, Juan Zhang, Xiaobo Li, Min Gao, Shuang-Nan Zhang, Zhi Zhang, Yu-Sa Wang, Li-Ming Song, Xufang Li, Liang Sun, Aimei Zhang, Tao Luo, Yu-Peng Chen, S. Xiao, Fangjun Lu, Li Chen, Shu Zhang, Guan-Hua Gao, Xiao-Fan Zhao, Ling-Jun Wang, N. Sai, He Gao, Q. Luo, Yifei Zhang, Bin Meng, Fan Zhang, Y. P. Chen, Mei Wu, Yu-Xuan Zhu, B. S. Liu, D. K. Zhou, Shu-Mei Jia, Ming-Yu Ge, Xiao-Jing Liu, Juan Wang, Xue-Feng Lu, Ge Ou, Chengmo Zhang, R. L. Zhuang, Hai-Sheng Zhao, C. X. Liu, Gang Chen, Yong Chen, Y. N. Liu, Y. Nang, Guang-Cheng Xiao, G. F. Wang, Jing-Kang Deng, Xiaohua Liang, Yuan You, Youli Tuo, Qi-Bin Yi, Bobing Wu, Ti-Pei Li, Y. J. Yang, Ying Tan, Zi-Liang Zhang, YongJie Jin, Yanji Yang, Yi Zhang, L. D. Kong, and Chen Wang

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Static timing analysis, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the observational results from a detailed timing analysis of the black hole candidate EXO 1846–031 during its outburst in 2019 with the observations of Insight-HXMT, NICER and MAXI. This outburst can be classified roughly into four different states. Type-C quasi-periodic oscillations (QPOs) observed by NICER (about 0.1–6 Hz) and Insight-HXMT (about 0.7–8 Hz) are also reported in this work. Meanwhile, we study various physical quantities related to QPO frequency. The QPO rms–frequency relationship in the energy band 1–10 keV indicates that there is a turning pointing in frequency around 2 Hz, which is similar to that of GRS 1915+105. A possible hypothesis for the relationship above may be related to the inclination of the source, which may require a high inclination to explain it. The relationships between QPO frequency and QPO rms, hardness, total fractional rms and count rate have also been found in other transient sources, which can indicate that the origin of type–C QPOs is non-thermal.

Published
2020

7. Discovery of oscillations above 200 keV in a black hole X-ray binary with Insight-HXMT

Author

Yu-Dong Gu, Yue Zhu, L. D. Kong, T. Luo, Chen Wang, Yanji Yang, Shaolin Xiong, Liang Zhang, Yi Zhang, Y. J. Yang, Zi-Liang Zhang, XiangYang Wen, Jia Huo, Hai-Sheng Zhao, Jing-Kang Deng, YongJie Jin, Jin-Yuan Liao, X. L. Cao, Fu-Guo Xie, Ju Guan, X. Y. Song, Mao-Shun Li, D. K. Zhou, Min-Xue Fu, Yu-Peng Chen, Xian Li, Y. P. Chen, Xiaohua Liang, Zheng-Wei Li, Yuan You, Hongwei Liu, Sheng Yang, Qi-Bin Yi, Luhua Jiang, Yanguo Li, Yuan-Yuan Du, Wei-Wei Cui, He Xu, Yu-Sa Wang, Yongjie Zhang, Li-Ming Song, Wan-Chang Zhang, Cheng-Cheng Guo, Wenshuai Wang, Li Chen, Zhi Zhang, Lian Tao, Y. Nang, Shu Zhang, Yongwei Dong, W. C. Jiang, Xue-Feng Lu, Xiao-Fan Zhao, Yue Zhang, Jianyin Nie, Shuo Xiao, Bo Lu, M. Gao, Xiaobo Li, G. F. Wang, Xiang Ma, Chengmo Zhang, Mei Wu, Guan-Hua Gao, Ying Tan, Shi-Jie Zheng, Tian-Xiang Chen, Qingcui Bu, Shu-Mei Jia, Qian-Qing Yin, Wen-Zhao Zhang, Ge Ou, Liang Sun, Bing Li, Jin-Lu Qu, B. B. Wu, Tong Zhang, Y. L. Tuo, Da-Wei Han, J. W. Yang, Juan Zhang, Long Ji, Feng Yuan, Jian-Feng Zhou, Guang-Cheng Xiao, R. L. Zhuang, Yupeng Xu, C. X. Liu, Wei Cui, Fangjun Lu, Jing Jin, Bobing Wu, He Gao, Zhi Chang, Juan Wang, Yifei Zhang, Ti-Pei Li, GuoQing Liu, Ming-Yu Ge, Xiao-Jing Liu, Fan Zhang, Qi Luo, Yong Chen, Yue Huang, Yu-Xuan Zhu, Shuang-Nan Zhang, Aimei Zhang, Cheng-Kui Li, Xufang Li, Gang Li, Wei Li, C. Cai, Zhao Zhang, N. Sai, Bin Meng, R. C. Shang, Gang Chen, Wei Zhang, Bai-Sheng Liu, Ling-Jun Wang, Hong-Mei Zhang, and Y. N. Liu

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Jet (fluid), Photon, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, law.invention, Black hole, Telescope, law, Quasiperiodic function, Precession, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Low-frequency quasi-periodic oscillations (LFQPOs) are commonly found in black hole X-ray binaries, and their origin is still under debate. The properties of LFQPOs at high energies (above 30 keV) are closely related to the nature of the accretion flow in the innermost regions, and thus play a crucial role in critically testing various theoretical models. The Hard X-ray Modulation Telescope (Insight-HXMT) is capable of detecting emissions above 30 keV, and is therefore an ideal instrument to do so. Here we report the discovery of LFQPOs above 200 keV in the new black hole MAXI J1820+070 in the X-ray hard state, which allows us to understand the behaviours of LFQPOs at hundreds of kiloelectronvolts. The phase lag of the LFQPO is constant around zero below 30 keV, and becomes a soft lag (that is, the high-energy photons arrive first) above 30 keV. The soft lag gradually increases with energy and reaches ~0.9s in the 150-200 keV band. The detection at energies above 200 keV, the large soft lag and the energy-related behaviors of the LFQPO pose a great challenge for most currently existing models, but suggest that the LFQPO probably originates from the precession of a small-scale jet., 36 pages, 12 figures, 3 tables; published in Nature Astronomy

Published
2020

8. Overview to the Hard X-ray Modulation Telescope (Insight-HXMT) Satellite

Author

Mao-Shun Li, YongJie Jin, Cheng-Kui Li, Xiaobo Li, ChunLei Zhang, Shaolin Xiong, C. L. Zou, ShiJie Zheng, C. Wang, W. C. Jiang, Min-Xue Fu, Yifei Zhang, Min Gao, Yu-Sa Wang, Tian-Xiang Chen, Wei Chen, Yuan-Yuan Du, Xufang Li, Jin-Lu Qu, Guan-Hua Gao, Yue Zhu, Shu-Mei Jia, Wei Li, J. W. Yang, Yue Zhang, Tong Zhang, N. Sai, Ming-Yu Ge, Xiao-Jing Liu, Tao Luo, WenHui Tao, Ge Ou, Wen-Zhao Zhang, Qiang Zhang, Juan Wang, Bing Li, Bin Yuan, Guang-Cheng Xiao, ShenYi Zhang, Zhao Zhang, Qi Luo, Bin Meng, Xiao-Fan Zhao, R. C. Shang, Liang Zhang, Bobing Wu, X. Y. Song, Yupeng Xu, Jianling Zhao, Da-Wei Han, Hai-Sheng Zhao, Wei Zhang, Yue Huang, Ti-Pei Li, Can Güngör, HongMei Zhang, Jing Jin, Cheng-Cheng Guo, C. Cai, Jianyin Nie, Wan-Chang Zhang, GuoHong Shen, XiangYang Wen, Shuo Xiao, Yongwei Dong, Yong Chen, Yanguo Li, R. L. Zhuang, C. X. Liu, Li-Ming Song, Wei Hu, Yan Huang, Jin-Yuan Liao, X. L. Cao, Bo Lu, Y. Nang, Yu-Peng Chen, Jing-Kang Deng, Xue-Feng Lu, JiaXi Yu, Xiaohua Liang, Wei-Wei Cui, Qingcui Bu, Shu Zhang, Huanyu Wang, Gang Chen, Chengmo Zhang, Ju Guan, G. F. Wang, Xiang Ma, Zhi Zhang, Youli Tuo, Qi-Bin Yi, Y. P. Chen, Y. N. Liu, Zhi Chang, He Xu, Li Chen, ZiJian Li, Ying Tan, L. Sun, Bai-Sheng Liu, Fangjun Lu, He Gao, Mei Wu, Fan Zhang, Jia Huo, Gang Li, Xian Li, Hongwei Liu, Sheng Yang, Yu-Xuan Zhu, Luhua Jiang, Yongjie Zhang, Lian Tao, Wei Cui, Juan Zhang, Shuang-Nan Zhang, Aimei Zhang, GuoQing Liu, Yu-Dong Gu, Zheng-Wei Li, Wenshuai Wang, ShaoZhen Liu, L. D. Kong, LinLi Yan, Yanji Yang, Yi Zhang, Yuan Liu, and Zi-Liang Zhang

Subjects
Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, General Physics and Astronomy, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, Calibration, Demodulation, Ground segment, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Remote sensing, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Payload, Astrophysics::Instrumentation and Methods for Astrophysics, Sky, Satellite, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst
Abstract

As China's first X-ray astronomical satellite, the Hard X-ray Modulation Telescope (HXMT), which was dubbed as Insight-HXMT after the launch on June 15, 2017, is a wide-band (1-250 keV) slat-collimator-based X-ray astronomy satellite with the capability of all-sky monitoring in 0.2-3 MeV. It was designed to perform pointing, scanning and gamma-ray burst (GRB) observations and, based on the Direct Demodulation Method (DDM), the image of the scanned sky region can be reconstructed. Here we give an overview of the mission and its progresses, including payload, core sciences, ground calibration/facility, ground segment, data archive, software, in-orbit performance, calibration, background model, observations and some preliminary results., 29 pages, 40 figures, 6 tables, to appear in Sci. China-Phys. Mech. Astron. arXiv admin note: text overlap with arXiv:1910.04434

Published
2020
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9. Switches between accretion structures during flares in 4U 1901+03

Author

Z. Chang, Fuqin Zhang, S. N. Zhang, Qiu-Yi Luo, Y. B. Chen, B. B. Wu, Tao Luo, Aimei Zhang, J. Y. Zhang, Ming-Yu Ge, Armin Nabizadeh, Y. G. Li, S. Xiao, Y. L. Tuo, J. W. Yang, L. Chen, Chun-sheng Zhang, Peng Zhang, Yu-Dong Gu, Sergey S. Tsygankov, C. K. Li, Y. J. Jin, J. Y. Nie, M. X. Fu, Yue Zhang, X. J. Liu, Luhua Jiang, Y. P. Xu, Zhao Zhang, G. C. Xiao, Bo Li, H. Xu, Yu-Xuan Zhu, J. Z. Wang, X. H. Liang, W. Z. Zhang, L. Sun, Z. W. Li, G. H. Gao, Yanji Yang, Wan-Chang Zhang, Weiguang Cui, C. Cai, F. J. Lu, Yunchao Liu, Qingcui Bu, X. L. Cao, B. S. Liu, Bin Meng, D. K. Zhou, Y. J. Yang, Shaolin Xiong, Wenxiong Li, Tian-Xiang Chen, Lian Tao, Yi Zhang, Y. J. Zhang, M. Wu, Andrea Santangelo, XiangYang Wen, Suleimanov, H. Gao, Z. Zhang, L. D. Kong, X. Y. Song, Long Ji, W. C. Zhang, Q. B. Yi, B. Y. Wu, Mao-Shun Li, Q. Q. Yin, You-Hong Zhang, H. W. Liu, N. Sai, Da-Wei Han, J. Y. Liao, H. M. Zhang, Zhi Zhang, Ya Fang Huang, Y. F. Zhang, Min Gao, X. B. Li, B. Lu, J. L. Qu, Yi-Qiao Dong, Wenhan Jiang, Cheng-Cheng Guo, Y. S. Wang, Doroshenko, Yuan-Yuan Du, C. Z. Liu, Y X Zhu, Y. P. Chen, Sisi Yang, Y. H. Tan, J. F. Zhou, J. Jin, Xin-Fu Zhao, R. C. Shang, Xuelong Li, J. Guan, GuoQing Liu, Jia Huo, Gang Li, Lorenzo Ducci, Wei Cui, T. Zhang, Li-Ming Song, Xue-Feng Lu, Shuinai Zhang, S. M. Jia, He-Yang Liu, Y. Nang, R. L. Zhuang, J. K. Deng, C. Wang, X. H. Ma, H. S. Zhao, Ti-Pei Li, P. J. Wang, G. F. Wang, W. S. Wang, Ge Ou, Gang Chen, Yuan You, X. X. Li, and S. J. Zheng

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Accretion (astrophysics), Spectral line, Beam pattern, Neutron star, Accretion rate, Pulsar, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Polar cap, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report on our analysis of the 2019 outburst of the X-ray accreting pulsar 4U 1901+03 observed with Insight-HXMT and NICER. Both spectra and pulse profiles evolve significantly in the decaying phase of the outburst. Dozens of flares are observed throughout the outburst. They are more frequent and brighter at the outburst peak. We find that the flares, which have a duration from tens to hundreds of seconds, are generally brighter than the persistent emission by a factor of $\sim$ 1.5. The pulse profile shape during the flares can be significantly different than that of the persistent emission. In particular, a phase shift is clearly observed in many cases. We interpret these findings as direct evidence of changes of the pulsed beam pattern, due to transitions between the sub- and super-critical accretion regimes on a short time scale. We also observe that at comparable luminosities the flares' pulse profiles are rather similar to those of the persistent emission. This indicates that the accretion on the polar cap of the neutron star is mainly determined by the luminosity, i.e., the mass accretion rate., 11 pages, 8 figures, accepted for publication in MNRAS

Published
2020

10. The influence of the Insight-HXMT/LE time response on timing analysis

Author

Li-Ming Song, D. K. Zhou, Yong Chen, Yu-Xuan Zhu, Xiaobo Li, Rui-Can Ma, Wei-Wei Cui, B. B. Wu, Fangjun Lu, Wei Hu, Wei Li, Xiao-Fan Zhao, Yanji Yang, Zi-Liang Zhang, Jia Huo, Cheng-Kui Li, Yupeng Xu, Yu-Sa Wang, Shu Zhang, Tian-Ming Li, Youli Tuo, Juan Wang, Guang-Cheng Xiao, Da-Wei Han, Tian-Xiang Chen, Wei Chen, Bo Lu, Jin-Lu Qu, Mao-Shun Li, H. W. Liu, and Shi-Jie Zheng

Subjects
Physics, Pulse (signal processing), Phase (waves), Spectral density, Static timing analysis, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Computational physics, Root mean square, Full width at half maximum, Space and Planetary Science, Frequency domain, Time domain, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

LE is the low energy telescope of Insight-HXMT. It uses swept charge devices (SCDs) to detect soft X-ray photons. The time response of LE is caused by the structure of SCDs. With theoretical analysis and Monte Carlo simulations we discuss the influence of LE time response (LTR) on the timing analysis from three aspects: the power spectral density, the pulse profile and the time lag. After the LTR, the value of power spectral density monotonously decreases with the increasing frequency. The power spectral density of a sinusoidal signal reduces by a half at frequency 536 Hz. The corresponding frequency for QPO signals is 458 Hz. The Root mean square (RMS) of QPOs holds the similar behaviour. After the LTR, the centroid frequency and full width at half maxima (FWHM) of QPOs signals do not change. The LTR reduces the RMS of pulse profiles and shifts the pulse phase. In the time domain, the LTR only reduces the peak value of the crosscorrelation function while it does not change the peak position. Thus it will not affect the result of the time lag. When considering the time lag obtained from two instruments and one among them is LE, a 1.18 ms lag is expected caused by the LTR. The time lag calculated in the frequency domain is the same as that in the time domain., Comment: 11 pages, 9 figures

Published
2020
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11. Hot disk of the Swift J0243.6+6124 revealed by Insight-HXMT

Author

J. K. Deng, X. H. Ma, B. B. Wu, Min Gao, Lian Tao, L. Chen, Yi-Yan Yang, X. Y. Song, C. L. Zhang, Xue-Feng Lu, Shuinai Zhang, H. S. Zhao, S. M. Jia, C. Z. Liu, M. X. Fu, Y. Nang, Ya Fang Huang, Tao Luo, Wan-Chang Zhang, Bin Meng, Mao-Shun Li, Sisi Yang, X. X. Li, L. J. Qu, J. Z. Wang, Y. L. Tuo, G. F. Wang, J. W. Yang, W. C. Jiang, Tian-Xiang Chen, Weiguang Cui, Qingcui Bu, Yunchao Liu, Y. J. Jin, L. M. Song, Sergey S. Tsygankov, Y. J. Yang, V. Doroshenko, Ti-Pei Li, F. Zhang, Yuan-Yuan Du, S. J. Zheng, Gang Chen, W. S. Wang, J. Y. Liao, H. M. Zhang, Junke Zhang, Wenxiong Li, Qing-He Zhang, Ge Ou, Da-Wei Han, XiangYang Wen, J. Y. Nie, Y. F. Zhang, Andrea Santangelo, Shaolin Xiong, Bo Lu, J. Jin, Y. J. Zhang, Xuchao Zhao, H. Gao, W. Z. Zhang, Wei Zhang, G. H. Gao, Yi-Qiao Dong, Y. H. Tan, Cheng-Cheng Guo, M. Wu, Y. Zhang, Fangjun Lu, Y. B. Chen, Alexander A. Mushtukov, Z. Zhang, Long Ji, Y. P. Chen, Bing Li, Y. S. Wang, T. Zhang, Chun-sheng Zhang, Xiaobo Li, W. Hu, X. F. Li, X. H. Liang, C. L. Zou, Z. L. Zhang, C. K. Li, G. C. Xiao, H. Xu, Y. X. Zhu, Z. W. Li, Ming-Yu Ge, Z. J. Li, ShaoZhen Liu, L. D. Kong, Yidong Xu, Yu-Dong Gu, S. N. Zhang, Jia Huo, Gang Li, X. L. Cao, J. Zhao, J. Guan, Aimei Zhang, GuoQing Liu, Wei Cui, Yu-Xuan Zhu, X. J. Liu, Liang Sun, Y. G. Li, Luhua Jiang, Z. Chang, Yujuan Liu, H. W. Liu, and N. Sai

Subjects
Swift, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Magnetosphere, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Pulsar, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, computer.programming_language, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Scattering, Spectral properties, Astronomy and Astrophysics, Accretion (astrophysics), Neutron star, Radiation pressure, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, computer
Abstract

We report on analysis of observations of the bright transient X-ray pulsar \src obtained during its 2017-2018 giant outburst with Insight-HXMT, \emph{NuSTAR}, and \textit{Swift} observatories. We focus on the discovery of a sharp state transition of the timing and spectral properties of the source at super-Eddington accretion rates, which we associate with the transition of the accretion disk to a radiation pressure dominated (RPD) state, the first ever directly observed for magnetized neutron star. This transition occurs at slightly higher luminosity compared to already reported transition of the source from sub- to super-critical accretion regime associate with onset of an accretion column. We argue that this scenario can only be realized for comparatively weakly magnetized neutron star, not dissimilar to other ultra-luminous X-ray pulsars (ULPs), which accrete at similar rates. Further evidence for this conclusion is provided by the non-detection of the transition to the propeller state in quiescence which strongly implies compact magnetosphere and thus rules out magnetar-like fields., Submitted to MNRAS

Published
2019
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12. Timing analysis of 2S 1417-624 observed with NICER and Insight-HXMT

Author

Tao Luo, J. Y. Zhang, B. B. Wu, G. H. Gao, Z. L. Zhang, Gang Chen, M. Wu, Y. Zhang, C. K. Li, Wei Zhang, Y. P. Chen, Y. H. Tan, Yi-Qiao Dong, H. Xu, Y. J. Jin, Victor Doroshenko, Shaolin Xiong, Z. W. Li, Cheng-Cheng Guo, F. J. Lu, Ya Fang Huang, Bo Li, Y. J. Zhang, J. Jin, J. K. Deng, H. Gao, L. Chen, Yi-Yan Yang, J. Y. Liao, H. M. Zhang, Tian-Xiang Chen, Yunchao Liu, XiangYang Wen, X. X. Li, Y. F. Zhang, X. B. Li, X. H. Ma, Can Güngör, Li-Ming Song, Xue-Feng Lu, Suo Liu, Xuchao Zhao, W. C. Zhang, Y. S. Wang, J. Zhao, Y. Nang, J. Y. Nie, S. J. Zheng, Mao-Shun Li, Lian Tao, X. H. Liang, L. Sun, Y. G. Li, Qing-He Zhang, Y. L. Tuo, Aimei Zhang, J. W. Yang, C. Z. Liu, S. M. Jia, X. Y. Song, Y. B. Chen, Luhua Jiang, W. Hu, L. J. Qu, H. W. Liu, Sisi Yang, Yu-Xuan Zhu, Z. Zhang, Long Ji, N. Sai, Yuan-Yuan Du, Chun-sheng Zhang, Wenhan Jiang, C. L. Zou, Yupeng Xu, X. J. Liu, X. L. Cao, Z. Chang, C. L. Zhang, Yujuan Liu, Wenxiong Li, B. Lu, S. N. Zhang, Andrea Santangelo, Y. X. Zhu, Ming-Yu Ge, Jia Huo, Gang Li, Lorenzo Ducci, Wei Cui, T. Zhang, W. Z. Zhang, Ti-Pei Li, Xuelong Li, J. Guan, Z. J. Li, L. D. Kong, GuoQing Liu, Bin Meng, Yu-Dong Gu, Y. J. Yang, G. C. Xiao, Fuqin Zhang, W. S. Wang, Ge Ou, Da-Wei Han, Min Gao, H. S. Zhao, M. X. Fu, J. Z. Wang, Weiguang Cui, G. F. Wang, and Qingcui Bu

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Accretion (meteorology), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Theoretical models, FOS: Physical sciences, Static timing analysis, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, 01 natural sciences, Luminosity, Magnetic field, QC Physics, Pulsar, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope
Abstract

We present a study of timing properties of the accreting pulsar 2S 1417-624 observed during its 2018 outburst, based on Swift/BAT, Fermi/GBM, Insight-HXMT and NICER observations. We report a dramatic change of the pulse profiles with luminosity. The morphology of the profile in the range 0.2-10.0keV switches from double to triple peaks at $\sim2.5$ $\rm \times 10^{37}{\it D}_{10}^2\ erg\ s^{-1}$ and from triple to quadruple peaks at $\sim7$ $\rm \times 10^{37}{\it D}_{10}^2\ erg\ s^{-1}$. The profile at high energies (25-100keV) shows significant evolutions as well. We explain this phenomenon according to existing theoretical models. We argue that the first change is related to the transition from the sub to the super-critical accretion regime, while the second to the transition of the accretion disc from the gas-dominated to the radiation pressure-dominated state. Considering the spin-up as well due to the accretion torque, this interpretation allows to estimate the magnetic field self-consistently at $\sim7\times 10^{12}$G., 7 pages, 4 figures, 1 tables, accepted for publication in MNRAS

Published
2019

13. Insight-HXMT observations of Swift J0243.6+6124 during its 2017-2018 outburst

Author

Min-Xue Fu, Yanguo Li, Y. N. Liu, Li-Ming Song, Yu-Sa Wang, Jianling Zhao, Wan-Chang Zhang, Victor Doroshenko, Wei Zhang, Xue-Feng Lu, Xiaobo Li, Zi-Liang Zhang, Cheng-Cheng Guo, Da-Wei Han, YongJie Jin, He Xu, C. L. Zou, C. L. Zhang, HongMei Zhang, Guang-Cheng Xiao, Yongwei Dong, Juan Zhang, Yifei Zhang, Li Chen, Can Güngör, ZiJian Li, Yue Zhang, ShaoZhen Liu, Jin-Yuan Liao, ChunLei Zhang, Jianyin Nie, Jing-Kang Deng, Shu Zhang, Yu-Dong Gu, Wei Hu, Tong Zhang, Ming-Yu Ge, Xiao-Jing Liu, Y. Nang, LuHua Jiang, Jin-Lu Qu, M. Gao, Yue Zhu, Xufang Li, J. W. Yang, Bo Lu, Xiao-Fan Zhao, Cheng-Kui Li, Ju Guan, Youli Tuo, Huanyu Wang, Changsheng Shi, T. Luo, Andrea Santangelo, G. F. Wang, Xiang Ma, Yongjie Zhang, N. Sai, Zheng-Wei Li, Hai-Sheng Zhao, W. C. Jiang, Bin Meng, Lian Tao, Gang Chen, Wei-Wei Cui, Ying Tan, Yue Huang, Shaolin Xiong, Tian-Xiang Chen, Wei Li, Zhao Zhang, Guan-Hua Gao, Shu-Mei Jia, Bobing Wu, W. Z. Zhang, W. S. Wang, Zhi Chang, Ge Ou, Liang Sun, Y. P. Chen, C. X. Liu, Bing Li, Yupeng Xu, Jing Jin, WenHui Tao, Juan Wang, H. T. Liu, Mao-Shun Li, L. L. Yan, ShiJie Zheng, Yanji Yang, Yuan-Yuan Du, Mei Wu, XiangYang Wen, Yi Zhang, Xian Li, Sheng Yang, Wei Cui, GuoQing Liu, Jia Huo, Yuan Liu, Gang Li, Long Ji, X. H. Liang, He Gao, Shuang-Nan Zhang, Aimei Zhang, Yong Chen, Fan Zhang, and Yu-Xuan Zhu

Subjects
Physics, Swift, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Accretion (astrophysics), Accretion disc, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, computer, Astrophysics::Galaxy Astrophysics, computer.programming_language
Abstract

The recently discovered neutron star transient Swift J0243.6+6124 has been monitored by {\it the Hard X-ray Modulation Telescope} ({\it Insight-\rm HXMT). Based on the obtained data, we investigate the broadband spectrum of the source throughout the outburst. We estimate the broadband flux of the source and search for possible cyclotron line in the broadband spectrum. No evidence of line-like features is, however, found up to $\rm 150~keV$. In the absence of any cyclotron line in its energy spectrum, we estimate the magnetic field of the source based on the observed spin evolution of the neutron star by applying two accretion torque models. In both cases, we get consistent results with $B\rm \sim 10^{13}~G$, $D\rm \sim 6~kpc$ and peak luminosity of $\rm >10^{39}~erg~s^{-1}$ which makes the source the first Galactic ultraluminous X-ray source hosting a neutron star., published

Published
2019
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14. Insight-HXMT observations of the New Black Hole Candidate MAXI J1535-571: timing analysis

Author

Wei Zhang, Yi-Qiao Dong, Cheng-Cheng Guo, X. L. Cao, Fu-Guo Xie, Xian Hou, Yupeng Xu, Jiancheng Wang, Xian Li, Jundan Nie, Y. G. Li, Yunchao Liu, Z. Chang, Yujuan Liu, C. L. Zou, Luhua Jiang, Y. J. Yang, W. C. Jiang, C. Z. Liu, Wei Cui, Mao-Shun Li, J. K. Deng, J. F. Zhou, Tianmeng Zhang, B. B. Wu, Jia Huo, X. H. Ma, Ju Guan, J. F. Ji, Xiaobo Li, ShaoZhen Liu, Tianran Chen, Shan-Shan Weng, Gang Chen, Yu-Dong Gu, Lian Tao, Y. X. Zhu, Li-Ming Song, Ming-Yu Ge, Xiao-Jing Liu, Bing Li, Guobao Zhang, Xue-Feng Lu, H. W. Liu, Shuinai Zhang, W. Z. Zhang, Yuan-Yuan Du, Z. L. Zhang, Y. S. Wang, Wenxiong Li, GuoQing Liu, Y. H. Tan, L. Chen, Wenfei Yu, Hsiang-Kuang Chang, S. N. Zhang, Chuan-Peng Zhang, Ya Fang Huang, Y. Nang, C. L. Zhang, Limei Yan, S. Yang, G. H. Gao, Wan-Chang Zhang, Y. P. Chen, Can Güngör, Y. B. Chen, Ti-Pei Li, M. Wu, Y. Zhang, G. F. Wang, Y. L. Tuo, J. Y. Liao, H. M. Zhang, J. W. Yang, Y. F. Zhang, Bo Lu, Xuchao Zhao, M. X. Fu, Jia Zhang, C. K. Li, H. Wang, Wei Hu, Z. Zhang, X. X. Li, Weiguang Cui, Qing-He Zhang, Zhuo Li, Qingcui Bu, Shu-Mei Jia, W. S. Wang, Shaolin Xiong, HongSheng Zhao, H. Xu, Ge Ou, Y. J. Zhang, Z. W. Li, Da-Wei Han, H. Gao, S. J. Zheng, Tao Luo, X. H. Liang, Min Gao, J. Zhao, J. L. Qu, Liang Sun, Albert K. H. Kong, Aimei Zhang, Gang Li, N. Sai, Yu-Xuan Zhu, Bin Meng, Fangjun Lu, Y. J. Jin, J. Jin, R. C. Shang, WenHui Tao, G. C. Xiao, F. Zhang, and XiangYang Wen

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Static timing analysis, Centroid, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Phase lag, law.invention, Black hole, Telescope, Amplitude, Space and Planetary Science, law, 0103 physical sciences, Modulation (music), Intermediate state, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract

We present the X-ray timing results of the new black hole candidate (BHC) MAXI J1535-571 during its 2017 outburst from Hard X-ray Modulation Telescope (\emph{Insight}-HXMT) observations taken from 2017 September 6 to 23. Following the definitions given by \citet{Belloni2010}, we find that the source exhibits state transitions from Low/Hard state (LHS) to Hard Intermediate state (HIMS) and eventually to Soft Intermediate state (SIMS). Quasi-periodic oscillations (QPOs) are found in the intermediate states, which suggest different types of QPOs. With the large effective area of \emph{Insight}-HXMT at high energies, we are able to present the energy dependence of the QPO amplitude and centroid frequency up to 100 keV which is rarely explored by previous satellites. We also find that the phase lag at the type-C QPOs centroid frequency is negative (soft lags) and strongly correlated with the centroid frequency. By assuming a geometrical origin of type-C QPOs, the source is consistent with being a high inclination system., Comment: 12 pages, 11 figures, Sumbitted to ApJ

Published
2018
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15. Insight-HXMT observations of the first binary neutron star merger GW170817

Author

Xufang Li, C. L. Zou, Yongjie Zhang, Yifei Zhang, Lian Tao, N. Sai, Ti-Pei Li, Shuang-Nan Zhang, Bin Meng, Aimei Zhang, Tong Zhang, Ming-Yu Ge, Xiao-Jing Liu, Yupeng Xu, Yuan Liu, Jing Jin, J. W. Yang, ShaoZhen Liu, Guan-Hua Gao, Xian Li, Sheng Yang, X. L. Cao, G. C. Xiao, Yong Chen, LinLi Yan, Shu-Mei Jia, Y. Tan, XiangYang Wen, W. C. Jiang, Yu-Dong Gu, Zheng-Wei Li, LuHua Jiang, L. Chen, M. X. Fu, W. S. Wang, Huanyu Wang, Wei-Wei Cui, Jianling Zhao, Yue Zhang, Yanji Yang, Juan Zhang, Yu-Xuan Zhu, Mao-Shun Li, Tian-Xiang Chen, Shaolin Xiong, Ju Guan, Jianyin Nie, Ge Ou, Wei Li, Cheng-Cheng Guo, Liang Sun, Bing Li, Wei Cui, Cheng-Kui Li, Yu-Peng Chen, Fan Zhang, H. Gao, Jin-Lu Qu, Yi Zhang, Yuan-Yuan Du, Wei Hu, Xiao-Fan Zhao, Yongwei Dong, Yue Huang, Gang Chen, X. H. Liang, Yue Zhu, Fangjun Lu, WenHui Tao, Hai-Sheng Zhao, He Xu, Juan Wang, H. T. Liu, Y. B. Chen, Youli Tuo, T. Luo, Jia Huo, W. Z. Zhang, ZiJian Li, Zhao Zhang, Gang Li, Yu-Sa Wang, Mei Wu, Shu Zhang, J. Y. Liao, Wei Zhang, Bo Lu, Y. N. Liu, Zi-Liang Zhang, Zhi Chang, GuoQing Liu, Da-Wei Han, HongMei Zhang, YongJie Jin, Y. Nang, ChunLei Zhang, G. F. Wang, Xiang Ma, Yanguo Li, Li-Ming Song, Xue-Feng Lu, M. Gao, Shi-Jie Zheng, Qiang Zhang, Bobing Wu, C. L. Zhang, C. X. Liu, J. K. Deng, Wan-Chang Zhang, and Xiaobo Li

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, General Physics and Astronomy, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Compact star, 01 natural sciences, LIGO, law.invention, Telescope, Neutron star, law, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, Gamma-ray burst, 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope
Abstract

Finding the electromagnetic (EM) counterpart of binary compact star merger, especially the binary neutron star (BNS) merger, is critically important for gravitational wave (GW) astronomy, cosmology and fundamental physics. On Aug. 17, 2017, Advanced LIGO and \textit{Fermi}/GBM independently triggered the first BNS merger, GW170817, and its high energy EM counterpart, GRB 170817A, respectively, resulting in a global observation campaign covering gamma-ray, X-ray, UV, optical, IR, radio as well as neutrinos. The High Energy X-ray telescope (HE) onboard \textit{Insight}-HXMT (Hard X-ray Modulation Telescope) is the unique high-energy gamma-ray telescope that monitored the entire GW localization area and especially the optical counterpart (SSS17a/AT2017gfo) with very large collection area ($\sim$1000 cm$^2$) and microsecond time resolution in 0.2-5 MeV. In addition, \textit{Insight}-HXMT quickly implemented a Target of Opportunity (ToO) observation to scan the GW localization area for potential X-ray emission from the GW source. Although it did not detect any significant high energy (0.2-5 MeV) radiation from GW170817, its observation helped to confirm the unexpected weak and soft nature of GRB 170817A. Meanwhile, \textit{Insight}-HXMT/HE provides one of the most stringent constraints (~10$^{-7}$ to 10$^{-6}$ erg/cm$^2$/s) for both GRB170817A and any other possible precursor or extended emissions in 0.2-5 MeV, which help us to better understand the properties of EM radiation from this BNS merger. Therefore the observation of \textit{Insight}-HXMT constitutes an important chapter in the full context of multi-wavelength and multi-messenger observation of this historical GW event., Comment: accepted by Science China - Physics, Mechanics & Astronomy. Planned to publish on Oct 17, but postponed due to a problem on pdf file

Published
2017
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16. Proton irradiation effect on SCDs

Author

Yu-Sa Wang, Yue Zhu, Yu Wang, Da-Wei Han, Mao-Shun Li, Guo-He Yin, Cheng-Kui Li, Bo Lu, Di Wu, Wei Hu, Zi-Liang Zhang, Yan Liu, Wei-Wei Cui, Jingbin Lu, Yong Chen, Tian-Xiang Chen, Zheng-Wei Li, Wei Li, Jia Huo, Xiao-Yan Liu, Juan Wang, Yupeng Xu, Ke-Yan Ma, Yanji Yang, and Yi Zhang

Subjects
Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, Materials science, Proton, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Charge (physics), Astrophysics::Cosmology and Extragalactic Astrophysics, Instrumentation and Detectors (physics.ins-det), Fluence, law.invention, Telescope, Operating temperature, law, Irradiation, Astrophysics::Earth and Planetary Astrophysics, Atomic physics, Nuclear Experiment (nucl-ex), Nuclear Experiment, Instrumentation, Energy (signal processing), Dark current
Abstract

The Low Energy X-ray Telescope is a main payload on the Hard X-ray Modulation Telescope satellite. The swept charge device is selected for the Low Energy X-ray Telescope. As swept charge devices are sensitive to proton irradiation, irradiation test was carried out on the HI-13 accelerator at the China Institute of Atomic Energy. The beam energy was measured to be 10 MeV at the SCD. The proton fluence delivered to the SCD was $3\times10^{8}\mathrm{protons}/\mathrm{cm}^{2}$ over two hours. It is concluded that the proton irradiation affects both the dark current and the charge transfer inefficiency of the SCD through comparing the performance both before and after the irradiation. The energy resolution of the proton-irradiated SCD is 212 eV@5.9 keV at $-60\,^{\circ}\mathrm{C}$, while it before irradiated is 134 eV. Moreover, better performance can be reached by lowering the operating temperature of the SCD on orbit.

Published
2014
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17. A linear calibration method on DNL error for energy spectrum

Author

Bo, Lu, Yan-Hong, Fu, Yong, Chen, Wei-Wei, Cui, Yu-Sa, Wang, Yu-Peng, Xu, Guo-He, Yin, Yan-Ji, Yang, Yi, Zhang, Jia, Huo, Wei, Li, Tian-Xiang, Cheng, Wei, Hu, Da-Wei, Han, Mao-Shun, Li, Juan, Wang, Yu, Wang, Xiao-Yang, Liu, Yue, Zhu, Zhong-Yi, Zhao, and Ya, Zhang

Subjects
Physics - Instrumentation and Detectors, FOS: Physical sciences, Instrumentation and Detectors (physics.ins-det), Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

A calibration method aimed for the differential nonlinearity (DNL) error of the Low Energy X-ray Instrument (LE) onboard the Hard X-ray Modulation Telescope (HXMT) is presented, which is independent with electronic systems used as testing platform and is only determined by the analog-to-digital converter (ADC) itself. Exploring this method, ADCs that are used within the flight model phase of HXMT-LE can be calibrated individually and independently by a non-destructive and low-cost way, greatly alleviating the complexity of the problem. As a result, the performance of the energy spectrum can be significantly improved, further more, noise reduced and resolution enhanced.

Published
2014
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