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1. Revisiting the dead time effects of Insight-HXMT/ME on timing analysis

Author

Tuo, Youli, Li, Xiaobo, Tan, Ying, Wu, Baiyang, Jiang, Weichun, Song, Liming, Qu, Jinlu, Gogate, Sudeep, Zhang, Shuang-Nan, and Santangelo, Andrea

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Dead time is a common instrumental effect of X-ray detectors which would alter the behavior of timing properties of astronomical signals, such as distorting the shape of power density spectra (PDS), affecting the root-mean-square of potential quasi-periodic oscillation signals, etc. We revisit the effects of the dead time of Medium Energy X-ray telescope (ME) onboard Insight-HXMT, based on the simulation of electronic read-out mechanism that causes the dead time, and the real data. We investigate dead time effects on the pulse profile as well as the Quasi-Periodic Oscillation (QPO) signals. The dead time coefficient suggests a linear correlation with the observed count rate in each phase bin of the pulse profile according to the simulation of periodic signal as well as the real data observed on Swift J0243.6+6124. The Fourier-amplitude-difference (FAD) method could well recover the intrinsic shape of the observed PDS in the case that the PDS is from two identical detectors. We apply this technique on ME, by splitting the 9 FPGA modules into 2 groups. The results indicate that the FAD technique suits the case when two groups of detectors are not largely different; and the recovered PDS of Sco X-1 observed by ME slightly enhances the significance of the previously known QPO signal, meanwhile the root-mean-square of QPO is significantly improved. We provide the FAD correction tool implemented in HXMTDAS for users in the future to better analyze QPO signals., Comment: 9 pages, 8 figures, accepted for publication in MNRAS main journal

Published
2024

2. An Insight-HXMT view of the mHz quasi-regular modulation phenomenon in the black hole X-ray binary 4U 1630-47

Author

Yang, Zi-Xu, Zhang, Liang, Huang, Yue, Bu, Qingcui, Zhang, Zhen, Liu, He-Xin, Yu, Wei, Wang, Peng-Ju, Zhao, Q. C., Tao, L., Qu, Jin-Lu, Zhang, Shu, Zhang, Shuang-Nan, Song, Liming, Lu, Fangjun, Cao, Xuelei, Chen, Li, Cai, Ce, Chang, Zhi, Chen, Tianxian, Chen, Yong, Chen, Yupeng, Chen, Yibao, Cui, Weiwei, Ding, Guoqiang, Du, Yuanyuan, Gao, GuanHua, Gao, He, Ge, Mingyu, Gu, Yudong, Guan, Ju, Guo, Chengcheng, Han, Dawei, Huo, Jia, Jia, Shumei, Jiang, Weichun, Jin, Jing, Kong, Lingda, Li, Bing, Li, Gang, Li, Wei, Li, Xian, Li, Xufang, Li, Zhengwei, Li, Chengkui, Lin, Lin, Liu, Congzhan, Li, Tipei, Li, Xiaobo, Liang, Xiaohua, Liao, Jinyuan, Liu, Hongwei, Liu, Xiaojing, Lu, Xuefeng, Luo, Qi, Luo, Tao, Ma, Binyuan, Ma, Ruican, Ma, Xiang, Meng, Bin, Nang, Yi, Nie, Jianyin, Ou, Ge, Ren, Xiaoqin, Sai, Na, Song, Xinying, Sun, Liang, Tan, Ying, Tuo, Youli, Wang, Chen, Wang, Wenshuai, Wang, Lingjun, Wang, Yusa, Wang, Jieshuang, Wen, Xiangyang, Wu, Bobing, Wu, Baiyang, Wu, Mei, Xiao, Shuo, Xu, Yupeng, Xiong, Shaolin, Yang, Sheng, Yang, Yanji, Yi, Qibin, Yin, Qianqing, You, Yuan, Zhang, Bing, Zhang, Fan, Zhang, Hongmei, Zhang, Juan, Zhang, Wanchang, Zhang, Wei, Zhang, Binbin, Zhang, Peng, Zhang, Yifei, Zhang, Yuanhang, Zhao, Haisheng, Zhao, Xiaofan, Zheng, Shijie, and Zhou, Dengke

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Here we report the spectral-timing results of the black hole X-ray binary 4U 1630-47 during its 2021 outburst using observations from the Hard X-ray Modulation Telescope. Type-C quasi-periodic oscillations (QPOs) in 1.6--4.2 Hz and quasi-regular modulation (QRM) near 60 mHz are detected during the outburst. The mHz QRM has a fractional rms of 10%--16% in the 8--35 keV energy band with a Q factor (frequency/width) of 2--4. Benefiting from the broad energy band of hxmt, we study the energy dependence of the 60 mHz QRM in 1--100 keV for the first time. We find that the fractional rms of the mHz QRM increases with photon energy, while the time lags of the mHz QRM are soft and decrease with photon energy. Fast recurrence of the mHz QRM, in a timescale of less than one hour, has been observed during the outburst. During this period, the corresponding energy spectra moderately change when the source transitions from the QRM state to the non-QRM state. The QRM phenomena also shows a dependence with the accretion rate. We suggest that the QRM could be caused by an unknown accretion instability aroused from the corona.

Published
2022
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3. Quasi-periodic oscillations of the X-ray burst from the magnetar SGR J1935+2154 and associated with the fast radio burst FRB 200428

Author

Li, Xiaobo, Ge, Mingyu, Lin, Lin, Zhang, Shuang-Nan, Song, Liming, Cao, Xuelei, Zhang, Bing, Lu, Fangjun, Xu, Yupeng, Xiong, Shaolin, Tuo, Youli, Tan, Ying, Jiang, Weichun, Qu, Jinlu, Zhang, Shu, Wang, Lingjun, Wang, Jieshuang, Zhang, Binbin, Zhang, Peng, Li, Chengkui, Liu, Congzhan, Li, Tipei, Bu, Qingcui, Cai, Ce, Chen, Yong, Chen, Yupeng, Chang, Zhi, Chen, Li, Chen, Tianxian, Chen, Yibao, Cui, Weiwei, Du, Yuanyuan, Gao, Guanhua, Gao, He, Gu, Yudong, Guan, Ju, Guo, Chengcheng, Han, Dawei, Huang, Yue, Huo, Jia, Jia, Shumei, Jin, Jing, Kong, Lingda, Li, Bing, Li, Gang, Li, Wei, Li, Xian, Li, Xufang, Li, Zhengwei, Liang, Xiaohua, Liao, Jinyuan, Liu, Hexin, Liu, Hongwei, Liu, Xiaojing, Lu, Xuefeng, Luo, Qi, Luo, Tao, Ma, Binyuan, Ma, Ruican, Ma, Xiang, Meng, Bin, Nang, Yi, Nie, Jianyin, Ou, Ge, Ren, Xiaoqin, Sai, Na, Song, Xinying, Sun, Liang, Tao, Lian, Wang, Chen, Wang, Pengju, Wang, Wenshuai, Wang, Yusa, Wen, Xiangyang, Wu, Bobing, Wu, Baiyang, Wu, Mei, Xiao, Shuo, Yang, Sheng, Yang, Yanji, Yi, Qibin, Yin, Qianqing, You, Yuan, Yu, Wei, Zhang, Fan, Zhang, Hongmei, Zhang, Juan, Zhang, Wanchang, Zhang, Wei, Zhang, Yifei, Zhang, Yuanhang, Zhao, Haisheng, Zhao, Xiaofan, Zheng, Shijie, and Zhou, Dengke

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

The origin(s) and mechanism(s) of fast radio bursts (FRBs), which are short radio pulses from cosmological distances, have remained a major puzzle since their discovery. We report a strong Quasi-Periodic Oscillation(QPO) of 40 Hz in the X-ray burst from the magnetar SGR J1935+2154 and associated with FRB 200428, significantly detected with the Hard X-ray Modulation Telescope (Insight-HXMT) and also hinted by the Konus-Wind data. QPOs from magnetar bursts have only been rarely detected; our 3.4 sigma (p-value is 2.9e-4) detection of the QPO reported here reveals the strongest QPO signal observed from magnetars (except in some very rare giant flares), making this X-ray burst unique among magnetar bursts. The two X-ray spikes coinciding with the two FRB pulses are also among the peaks of the QPO. Our results suggest that at least some FRBs are related to strong oscillation processes of neutron stars. We also show that we may overestimate the significance of the QPO signal and underestimate the errors of QPO parameters if QPO exists only in a fraction of the time series of a X-ray burst which we use to calculate the Leahy-normalized periodogram., Comment: 17 pages, 13 figures, accepted for publication by ApJ. arXiv admin note: text overlap with arXiv:1212.1011 by other authors. text overlap with arXiv:1212.1011 by other authors

Published
2022
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4. The removal method and generation mechanism of spikes in Insight-HXMT/HE telescope

Author

Wu, Baiyang, Zhang, Yifei, Li, Xiaobo, Zhao, Haisheng, Ge, Mingyu, Liu, Congzhan, Song, Liming, and Qu, Jinlu

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Spikes are some obvious sharp increases that appear on the raw light curves of High Energy X-ray telescope(HE) onboard Insight-HXMT, which could have influences on the data products like energy and power spectra. They are considered to be fake triggers generated by large signals. In this paper, we study the characteristic of the spikes and propose two methods to remove spikes from the raw data. According to the different influences on energy and power spectra, the best parameters for removing the spikes is selected and used in the Insight-HXMT data analysis software. The generation mechanism of spikes is also studied using the backup HE detectors on ground and the spikes can be reduced by the electronic design.

Published
2022
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5. In-orbit timing calibration of the Insight-Hard X-ray Modulation Telescope

Author

Tuo, Youli, Li, Xiaobo, Ge, Mingyu, Nie, Jianyin, Song, Liming, Xu, Yupeng, Zheng, Shijie, Lu, Fangjun, Zhang, Shuang-Nan, Liu, Congzhan, Cao, Xuelei, Chen, Yong, Qu, Jinlu, Zhang, Shu, Zhao, Haisheng, Xiao, Shuo, Wu, Baiyang, Wen, Xiangyang, Jiang, Weichun, Meng, Bin, Cui, Weiwei, Li, Wei, Zhang, Yifei, Li, Xufang, Yang, Yanji, Tan, Ying, and Li, Bing

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We describe the timing system and the timing calibration results of the three payloads on-board the Insight-Hard X-ray Modulation Telescope (Insight-HXMT). These three payloads are the High Energy X-ray telescope (HE, 20-250 keV), the Medium Energy X-ray telescope (ME, 5-30 keV) and the low Energy X-ray telescope (LE, 1-10 keV). We present a method to correct the temperature-dependent period response and the long-term variation of the on-board crystal oscillator, especially for ME that does not carry a temperature-compensated crystal oscillator. The time of arrivals (ToAs) of the Crab pulsar are measured to evaluate the accuracy of the timing system. As the ephemeris of the Crab pulsar given by Jodrell Bank observatory has systematic errors around 40 {\mu}s (Rots et al. 2014), we use the quasi-simultaneous observations of the X-ray Timing Instrument (XTI) on-board the Neutron star Interior Composition Explorer (NICER) to produce the Crab ephemerides and to verify the timing system of Insight-HXMT. The energy-dependent ToAs' offsets relative to the NICER measurements including physical and instrumental origins are about 24.7{\mu}s, 10.1{\mu}s and 864.7{\mu}s, and the systematic errors of the timing system are determined as 12.1{\mu}s, 8.6{\mu}s, and 15.8{\mu}s, for HE, ME and LE respectively., Comment: 29 pages, 14 figures, accepted for publication in ApJS

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

Author

You, Bei, Tuo, Yuoli, Li, Chengzhe, Wang, Wei, Zhang, Shuang-Nan, Zhang, Shu, Ge, Mingyu, Luo, Chong, Liu, Bifang, Yuan, Weimin, Dai, Zigao, Liu, Jifeng, Qiao, Erlin, Jin, Chichuan, Liu, Zhu, Czerny, Bozena, Wu, Qingwen, Bu, Qingcui, Cai, Ce, Cao, Xuelei, Chang, Zhi, Chen, Gang, Chen, Li, Chen, Tianxiang, Chen, Yibao, Chen, Yong, Chen, Yupeng, Cui, Wei, Cui, Weiwei, Deng, Jingkang, Dong, Yongwei, Du, Yuanyuan, Fu, Minxue, Gao, Guanhua, Gao, He, Gao, Min, Gu, Yudong, Guan, Ju, Guo, Chengcheng, Han, Dawei, Huang, Yue, Huo, Jia, Jia, Shumei, Jiang, Luhua, Jiang, Weichun, Jin, Jing, Jin, Yongjie, Kong, Lingda, Li, Bing, Li, Chengkui, Li, Gang, Li, Maoshun, Li, Tipei, Li, Wei, Li, Xian, Li, Xiaobo, Li, Xufang, Li, Yanguo, Li, Zhengwei, Liang, Xiaohua, Liao, Jinyuan, Liu, Congzhan, Liu, Guoqing, Liu, Hongwei, Liu, Xiaojing, Liu, Yinong, Lu, Bo, Lu, Fangjun, Lu, Xuefeng, Luo, Qi, Luo, Tao, Ma, Xiang, Meng, Bin, Nang, Yi, Nie, Jianyin, Ou, Ge, Qu, Jinlu, Sai, Na, Shang, Rencheng, Song, Liming, Song, Xinying, Sun, Liang, Tan, Ying, Tao, Lian, Wang, Chen, Wang, Guofeng, Wang, Juan, Wang, Lingjun, Wang, Wenshuai, Wang, Yusa, Wen, Xiangyang, Wu, Baiyang, Wu, Bobing, Wu, Mei, Xiao, Guangcheng, Xiao, Shuo, Xiong, Shaolin, Xu, Yupeng, Yang, Jiawei, Yang, Sheng, Yang, Yanji, Yi, Qibin, Yin, Qianqing, You, Yuan, Zhang, Aimei, Zhang, Chengmo, Zhang, Fan, Zhang, Hongmei, Zhang, Juan, Zhang, Tong, Zhang, Wanchang, Zhang, Wei, Zhang, Wenzhao, Zhang, Yi, Zhang, Yifei, Zhang, Yongjie, Zhang, Yue, Zhang, Zhao, Zhang, Ziliang, Zhao, Haisheng, Zhao, Xiaofan, Zheng, Shijie, Zhou, Dengke, Zhou, Jianfeng, Zhu, Yuxuan, and Zhu, Yue

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
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., Comment: 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
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7. In-flight calibration of the Insight-Hard X-ray Modulation Telescope

Author

Li, Xiaobo, Li, Xufang, Tan, Ying, Yang, Yanji, Ge, Mingyu, Zhang, Juan, Tuo, Youli, Wu, Baiyang, Liao, Jinyuan, Zhang, Yifei, Song, Liming, Zhang, Shu, Qu, Jinlu, Zhang, Shuang-nan, Lu, Fangjun, Xu, Yupeng, Liu, Congzhan, Cao, Xuelei, Chen, Yong, Nie, Jianyin, Zhao, Haisheng, and Li, Chengkui

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present the calibration of the Insight-Hard X-ray Modulation Telescope (Insight-HXMT) X-ray satellite, which can be used to perform timing and spectral studies of bright X-ray sources. Insight-HXMT carries three main payloads onboard: the High Energy X-ray telescope (HE), the Medium Energy X-ray telescope (ME) and the Low Energy X-ray telescope (LE). In orbit, the radioactive sources, activated lines, the fluorescence lines and celestial sources are used to calibrate the energy scale and energy resolution of the payloads. The Crab nebular is adopted as the primary effective area calibrator and empirical functions are constructed to modify the simulated effective areas of the three payloads respectively. The systematic errors of HE, compared to the model of the Crab nebular, are less than 2% in 28--120 keV and 2%--10% above 120 keV. The systematic errors of ME are less than 1.5% in 10--35 keV. The systematic errors of LE are less than 1% in 1--7 keV except the Si K--edge (1.839 keV, up to 1.5%) and less than 2% in 7--10 keV., Comment: 14 pages, 28 figures, accepted by Journal of High Energy Astrophysics

Published
2020

8. A Method of Realizing Adaptive Uniform Illumination by Pyramid Prism for PA-LiDAR.

Author

Zhang, Shuo, Wu, Baiyang, Bi, Yong, and Gao, Weinan

Abstract

In this paper, we propose a simple method to generate the uniform illumination using a pyramid prism for Plane Array Laser Imaging Detection and Ranging (PA-LiDAR). The principle of the pyramid prism shaping the Gaussian beam to form a uniform beam was analyzed theoretically. By changing the parameters of the pyramid prism and laser beam, the profile distribution of the output beam can be easily adjusted. Based on the operation mode and illumination requirements of PA-LiDAR, we have developed a set of LiDAR prototypes using a pyramid prism and carried out experimental research on these prototypes. The simulation and experimental results demonstrated that this method can achieve a uniform illumination beam with excellent propagation properties for meeting the technical requirements of PA-LiDAR. This method of uniform illumination has the advantages of being simple, flexible, easily adjustable and convenient to operate. [ABSTRACT FROM AUTHOR]

Published
2024
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9. A Method for Fingerprint Edge Enhancement Based on Radial Hilbert Transform.

Author

Wu, Baiyang, Zhang, Shuo, Gao, Weinan, Bi, Yong, and Hu, Xiaosong

Subjects
HILBERT transform, ENTROPY (Information theory), SIGNAL-to-noise ratio, IMAGE processing
Abstract

Fingerprints play a significant role in various fields due to their uniqueness. In order to effectively utilize fingerprint information, it is necessary to enhance image quality. This paper introduces a method based on Radial Hilbert transform (RHLT), which simulates the vortex filter using the point spread function (PSF) of spiral phase plate (SPP) with a topological charge l = 1 , for fingerprint edge enhancement. The experimental results show that the processed fingerprint image has more distinct edges, with an increase in information entropy and average gradient. Unlike classical edge detection operators, the fingerprint edge image obtained by the RHLT method exhibits a lower mean square error ( M S E ) and a higher peak signal-to-noise ratio ( P S N R ). This indicates that the RHLT method provides more accurate edge detection and demonstrates higher noise-resistance capabilities. Due to its ability to highlight edge information while preserving more original features, this method has great application potential in fingerprint image processing. [ABSTRACT FROM AUTHOR]

Published
2024
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11. Overview to the Hard X-ray Modulation Telescope (Insight-HXMT) Satellite

Author

Zhang, Shuang-Nan, Li, TiPei, Lu, FangJun, Song, LiMing, Xu, YuPeng, Liu, CongZhan, Chen, Yong, Cao, XueLei, Bu, QingCui, Chang, Zhi, Chen, Gang, Chen, Li, Chen, TianXiang, Chen, YiBao, Chen, YuPeng, Cui, Wei, Cui, WeiWei, Deng, JingKang, Dong, YongWei, Du, YuanYuan, Fu, MinXue, Gao, GuanHua, Gao, He, Gao, Min, Ge, MingYu, Gu, YuDong, Guan, Ju, Gungor, Can, Guo, ChengCheng, Han, DaWei, Hu, Wei, Huang, Yue, Huo, Jia, Jia, ShuMei, Jiang, LuHua, Jiang, WeiChun, Jin, Jing, Jin, YongJie, Li, Bing, Li, ChengKui, Li, Gang, Li, MaoShun, Li, Wei, Li, Xian, Li, XiaoBo, Li, XuFang, Li, YanGuo, Li, ZiJian, Li, ZhengWei, Liang, XiaoHua, Liao, JinYuan, Liu, GuoQing, Liu, HongWei, Liu, ShaoZhen, Liu, XiaoJing, Liu, Yuan, Liu, YiNong, Lu, Bo, Lu, XueFeng, Luo, Tao, Ma, Xiang, Meng, Bin, Nang, Yi, Nie, JianYin, Ou, Ge, Qu, JinLu, Sai, Na, Shang, RenCheng, Shen, GuoHong, Sun, Liang, Tan, Ying, Tao, Lian, Tuo, YouLi, Wang, Chen, Wang, ChunQin, Wang, GuoFeng, Wang, HuanYu, Wang, Juan, Wang, WenShuai, Wang, YuSa, Wen, XiangYang, Wu, BaiYang, Wu, BoBing, Wu, Mei, Xiao, GuangCheng, Xiong, ShaoLin, Yan, LinLi, Yang, JiaWei, Yang, Sheng, Yang, YanJi, Yi, QiBin, Yuan, Bin, Zhang, AiMei, Zhang, ChunLei, Zhang, ChengMo, Zhang, Fan, Zhang, HongMei, Zhang, Juan, Zhang, Qiang, Zhang, ShenYi, Zhang, Shu, Zhang, Tong, Zhang, WanChang, Zhang, Wei, Zhang, WenZhao, Zhang, Yi, Zhang, YiFei, Zhang, YongJie, Zhang, Yue, Zhang, Zhao, Zhang, Zhi, Zhang, ZiLiang, Zhao, HaiSheng, Zhao, XiaoFan, Zheng, ShiJie, Zhou, JianFeng, Zhu, YuXuan, Zhu, Yue, and Zhuang, RenLin

Published
2020
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12. An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630–47

Author

Yang, Zi-xu, primary, Zhang, Liang, additional, Huang, Yue, additional, Bu, Qingcui, additional, Zhang, Zhen, additional, Liu, He-Xin, additional, Yu, Wei, additional, Wang, Peng-Ju, additional, Zhao, Q. C., additional, Tao, L., additional, Qu, Jin-Lu, additional, Zhang, Shu, additional, Zhang, Shuang-Nan, additional, Song, Liming, additional, Lu, Fangjun, additional, Cao, Xuelei, additional, Chen, Li, additional, Cai, Ce, additional, Chang, Zhi, additional, Chen, Tianxiang, additional, Chen, Yong, additional, Chen, Yupeng, additional, Chen, Yibao, additional, Cui, Weiwei, additional, Ding, Guoqiang, additional, Du, Yuanyuan, additional, Gao, Guanhua, additional, Gao, He, additional, Ge, Mingyu, additional, Gu, Yudong, additional, Guan, Ju, additional, Guo, Chengcheng, additional, Han, Dawei, additional, Huo, Jia, additional, Jia, Shumei, additional, Jiang, Weichun, additional, Jin, Jing, additional, Kong, Lingda, additional, Li, Bing, additional, Li, Gang, additional, Li, Wei, additional, Li, Xian, additional, Li, Xufang, additional, Li, Zhengwei, additional, Li, Chengkui, additional, Lin, Lin, additional, Liu, Congzhan, additional, Li, Tipei, additional, Li, Xiaobo, additional, Liang, Xiaohua, additional, Liao, Jinyuan, additional, Liu, Hongwei, additional, Liu, Xiaojing, additional, Lu, Xuefeng, additional, Luo, Qi, additional, Luo, Tao, additional, Ma, Binyuan, additional, Ma, RuiCan, additional, Ma, Xiang, additional, Meng, Bin, additional, Nang, Yi, additional, Nie, Jianyin, additional, Ou, Ge, additional, Ren, Xiaoqin, additional, Sai, Na, additional, Song, Xinying, additional, Sun, Liang, additional, Tan, Ying, additional, Tuo, Youli, additional, Wang, Chen, additional, Wang, Wenshuai, additional, Wang, Lingjun, additional, Wang, Yusa, additional, Wang, Jieshuang, additional, Wen, Xiangyang, additional, Wu, Bobing, additional, Wu, Baiyang, additional, Wu, Mei, additional, Xiao, Shuo, additional, Xu, Yupeng, additional, Xiong, Shaolin, additional, Yang, Sheng, additional, Yang, Yanji, additional, Yi, Qibin, additional, Yin, Qianqing, additional, You, Yuan, additional, Zhang, Bing, additional, Zhang, Fan, additional, Zhang, Hongmei, additional, Zhang, Juan, additional, Zhang, Wanchang, additional, Zhang, Wei, additional, Zhang, Binbin, additional, Zhang, Peng, additional, Zhang, Yifei, additional, Zhang, Yuanhang, additional, Zhao, Haisheng, additional, Zhao, Xiaofan, additional, Zheng, Shijie, additional, and Zhou, Dengke, additional

Published
2022
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13. Quasi-periodic Oscillations of the X-Ray Burst from the Magnetar SGR J1935–2154 and Associated with the Fast Radio Burst FRB 200428

Author

Li, Xiaobo, primary, Ge, Mingyu, additional, Lin, Lin, additional, Zhang, Shuang-Nan, additional, Song, Liming, additional, Cao, Xuelei, additional, Zhang, Bing, additional, Lu, Fangjun, additional, Xu, Yupeng, additional, Xiong, Shaolin, additional, Tuo, Youli, additional, Tan, Ying, additional, Jiang, Weichun, additional, Qu, Jinlu, additional, Zhang, Shu, additional, Wang, Lingjun, additional, Wang, Jieshuang, additional, Zhang, Binbin, additional, Zhang, Peng, additional, Li, Chengkui, additional, Liu, Congzhan, additional, Li, Tipei, additional, Bu, Qingcui, additional, Cai, Ce, additional, Chen, Yong, additional, Chen, Yupeng, additional, Chang, Zhi, additional, Chen, Li, additional, Chen, Tianxiang, additional, Chen, Yibao, additional, Cui, Weiwei, additional, Du, Yuanyuan, additional, Gao, Guanhua, additional, Gao, He, additional, Gu, Yudong, additional, Guan, Ju, additional, Guo, Chengcheng, additional, Han, Dawei, additional, Huang, Yue, additional, Huo, Jia, additional, Jia, Shumei, additional, Jin, Jing, additional, Kong, Lingda, additional, Li, Bing, additional, Li, Gang, additional, Li, Wei, additional, Li, Xian, additional, Li, Xufang, additional, Li, Zhengwei, additional, Liang, Xiaohua, additional, Liao, Jinyuan, additional, Liu, Hexin, additional, Liu, Hongwei, additional, Liu, Xiaojing, additional, Lu, Xuefeng, additional, Luo, Qi, additional, Luo, Tao, additional, Ma, Binyuan, additional, Ma, Ruican, additional, Ma, Xiang, additional, Meng, Bin, additional, Nang, Yi, additional, Nie, Jianyin, additional, Ou, Ge, additional, Ren, Xiaoqin, additional, Sai, Na, additional, Song, Xinying, additional, Sun, Liang, additional, Tao, Lian, additional, Wang, Chen, additional, Wang, Pengju, additional, Wang, Wenshuai, additional, Wang, Yusa, additional, Wen, Xiangyang, additional, Wu, Bobing, additional, Wu, Baiyang, additional, Wu, Mei, additional, Xiao, Shuo, additional, Yang, Sheng, additional, Yang, Yanji, additional, Yi, Qibin, additional, Yin, Qianqing, additional, You, Yuan, additional, Yu, Wei, additional, Zhang, Fan, additional, Zhang, Hongmei, additional, Zhang, Juan, additional, Zhang, Wanchang, additional, Zhang, Wei, additional, Zhang, Yifei, additional, Zhang, Yuanhang, additional, Zhao, Haisheng, additional, Zhao, Xiaofan, additional, Zheng, Shijie, additional, and Zhou, Dengke, additional

Published
2022
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15. In-orbit Timing Calibration of the Insight-Hard X-Ray Modulation Telescope

Author

Tuo, Youli, primary, Li, Xiaobo, additional, Ge, Mingyu, additional, Nie, Jianyin, additional, Song, Liming, additional, Xu, Yupeng, additional, Zheng, Shijie, additional, Lu, Fangjun, additional, Zhang, Shuang-Nan, additional, Liu, Congzhan, additional, Cao, Xuelei, additional, Chen, Yong, additional, Qu, Jinlu, additional, Zhang, Shu, additional, Zhao, Haisheng, additional, Xiao, Shuo, additional, Wu, Baiyang, additional, Wen, Xiangyang, additional, Jiang, Weichun, additional, Meng, Bin, additional, Cui, Weiwei, additional, Li, Wei, additional, Zhang, Yifei, additional, Li, Xufang, additional, Yang, Yanji, additional, Tan, Ying, additional, and Li, Bing, additional

Published
2022
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16. Insight-HXMT observations of jet-like corona in a black hole X-ray binary MAXI J1820+070

Author

You, Bei, primary, Tuo, Yuoli, additional, Li, Chengzhe, additional, Wang, Wei, additional, Zhang, Shuang-Nan, additional, Zhang, Shu, additional, Ge, Mingyu, additional, Luo, Chong, additional, Liu, Bifang, additional, Yuan, Weimin, additional, Dai, Zigao, additional, Liu, Jifeng, additional, Qiao, Erlin, additional, Jin, Chichuan, additional, Liu, Zhu, additional, Czerny, Bozena, additional, Wu, Qingwen, additional, Bu, Qingcui, additional, Cai, Ce, additional, Cao, Xuelei, additional, Chang, Zhi, additional, Chen, Gang, additional, Chen, Li, additional, Chen, Tianxiang, additional, Chen, Yibao, additional, Chen, Yong, additional, Chen, Yupeng, additional, Cui, Wei, additional, Cui, Weiwei, additional, Deng, Jingkang, additional, Dong, Yongwei, additional, Du, Yuanyuan, additional, Fu, Minxue, additional, Gao, Guanhua, additional, Gao, He, additional, Gao, Min, additional, Gu, Yudong, additional, Guan, Ju, additional, Guo, Chengcheng, additional, Han, Dawei, additional, Huang, Yue, additional, Huo, Jia, additional, Jia, Shumei, additional, Jiang, Luhua, additional, Jiang, Weichun, additional, Jin, Jing, additional, Jin, Yongjie, additional, Kong, Lingda, additional, Li, Bing, additional, Li, Chengkui, additional, Li, Gang, additional, Li, Maoshun, additional, Li, Tipei, additional, Li, Wei, additional, Li, Xian, additional, Li, Xiaobo, additional, Li, Xufang, additional, Li, Yanguo, additional, Li, Zhengwei, additional, Liang, Xiaohua, additional, Liao, Jinyuan, additional, Liu, Congzhan, additional, Liu, Guoqing, additional, Liu, Hongwei, additional, Liu, Xiaojing, additional, Liu, Yinong, additional, Lu, Bo, additional, Lu, Fangjun, additional, Lu, Xuefeng, additional, Luo, Qi, additional, Luo, Tao, additional, Ma, Xiang, additional, Meng, Bin, additional, Nang, Yi, additional, Nie, Jianyin, additional, Ou, Ge, additional, Qu, Jinlu, additional, Sai, Na, additional, Shang, Rencheng, additional, Song, Liming, additional, Song, Xinying, additional, Sun, Liang, additional, Tan, Ying, additional, Tao, Lian, additional, Wang, Chen, additional, Wang, Guofeng, additional, Wang, Juan, additional, Wang, Lingjun, additional, Wang, Wenshuai, additional, Wang, Yusa, additional, Wen, Xiangyang, additional, Wu, Baiyang, additional, Wu, Bobing, additional, Wu, Mei, additional, Xiao, Guangcheng, additional, Xiao, Shuo, additional, Xiong, Shaolin, additional, Xu, Yupeng, additional, Yang, Jiawei, additional, Yang, Sheng, additional, Yang, Yanji, additional, Yi, Qibin, additional, Yin, Qianqing, additional, You, Yuan, additional, Zhang, Aimei, additional, Zhang, Chengmo, additional, Zhang, Fan, additional, Zhang, Hongmei, additional, Zhang, Juan, additional, Zhang, Tong, additional, Zhang, Wanchang, additional, Zhang, Wei, additional, Zhang, Wenzhao, additional, Zhang, Yi, additional, Zhang, Yifei, additional, Zhang, Yongjie, additional, Zhang, Yue, additional, Zhang, Zhao, additional, Zhang, Ziliang, additional, Zhao, Haisheng, additional, Zhao, Xiaofan, additional, Zheng, Shijie, additional, Zhou, Dengke, additional, Zhou, Jianfeng, additional, Zhu, Yuxuan, additional, and Zhu, Yue, additional

Published
2021
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17. In-flight calibration of the Insight-Hard X-ray Modulation Telescope

Author

Li, Xiaobo, primary, Li, Xufang, additional, Tan, Ying, additional, Yang, Yanji, additional, Ge, Mingyu, additional, Zhang, Juan, additional, Tuo, Youli, additional, Wu, Baiyang, additional, Liao, Jinyuan, additional, Zhang, Yifei, additional, Song, Liming, additional, Zhang, Shu, additional, Qu, Jinlu, additional, Zhang, Shuang-nan, additional, Lu, Fangjun, additional, Xu, Yupeng, additional, Liu, Congzhan, additional, Cao, Xuelei, additional, Chen, Yong, additional, Nie, Jianyin, additional, Zhao, Haisheng, additional, and Li, Chengkui, additional

Published
2020
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