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6. Insight-HXMT and GECAM-C observations of the brightest-of-all-time GRB 221009A

Author

An, Zheng-Hua, Antier, S., Bi, Xing-Zi, Bu, Qing-Cui, Cai, Ce, Cao, Xue-Lei, Camisasca, Anna-Elisa, Chang, Zhi, Chen, Gang, Chen, Li, Chen, Tian-Xiang, Chen, Wen, Chen, Yi-Bao, Chen, Yong, Chen, Yu-Peng, Coughlin, Michael W., Cui, Wei-Wei, Dai, Zi-Gao, Hussenot-Desenonges, T., Du, Yan-Qi, Du, Yuan-Yuan, Du, Yun-Fei, Fan, Cheng-Cheng, Frontera, Filippo, Gao, He, Gao, Min, Ge, Ming-Yu, Gong, Ke, Gu, Yu-Dong, Guan, Ju, Guo, Dong-Ya, Guo, Zhi-Wei, Guidorzi, Cristiano, Han, Da-Wei, He, Jian-Jian, He, Jun-Wang, Hou, Dong-Jie, Huang, Yue, Huo, Jia, Ji, Zhen, Jia, Shu-Mei, Jiang, Wei-Chun, Kann, David Alexander, Klotz, A., Kong, Ling-Da, Lan, Lin, Li, An, Li, Bing, Li, Chao-Yang, Li, Cheng-Kui, Li, Gang, Li, Mao-Shun, Li, Ti-Pei, Li, Wei, Li, Xiao-Bo, Li, Xin-Qiao, Li, Xu-Fang, Li, Yan-Guo, Li, Zheng-Wei, Liang, Jing, Liang, Xiao-Hua, Liao, Jin-Yuan, Lin, Lin, Liu, Cong-Zhan, Liu, He-Xin, Liu, Hong-Wei, Liu, Jia-Cong, Liu, Xiao-Jing, Liu, Ya-Qing, Liu, Yu-Rong, Lu, Fang-Jun, Lu, Hong, Lu, Xue-Feng, Luo, Qi, Luo, Tao, Ma, Bin-Yuan, Ma, Fu-Li, Ma, Rui-Can, Ma, Xiang, Maccary, Romain, Mao, Ji-Rong, Meng, Bin, Nie, Jian-Yin, Orlandini, Mauro, Ou, Ge, Peng, Jing-Qiang, Peng, Wen-Xi, Qiao, Rui, Qu, Jin-Lu, Ren, Xiao-Qin, Shi, Jing-Yan, Shi, Qi, Song, Li-Ming, Song, Xin-Ying, Su, Ju, Sun, Gong-Xing, Sun, Liang, Sun, Xi-Lei, Tan, Wen-Jun, Tan, Ying, Tao, Lian, Tuo, You-Li, Turpin, Damien, Wang, Jin-Zhou, Wang, Chen, Wang, Chen-Wei, Wang, Hong-Jun, Wang, Hui, Wang, Jin, Wang, Ling-Jun, Wang, Peng-Ju, Wang, Ping, Wang, Wen-Shuai, Wang, Xiang-Yu, Wang, Xi-Lu, Wang, Yu-Sa, Wang, Yue, Wen, Xiang-Yang, Wu, Bo-Bing, Wu, Bai-Yang, Wu, Hong, Xiao, Sheng-Hui, Xiao, Shuo, Xiao, Yun-Xiang, Xie, Sheng-Lun, Xiong, Shao-Lin, Xiong, Sen-Lin, Xu, Dong, Xu, He, Xu, Yan-Jun, Xu, Yan-Bing, Xu, Ying-Chen, Xu, Yu-Peng, Xue, Wang-Chen, Yang, Sheng, Yang, Yan-Ji, Yang, Zi-Xu, Ye, Wen-Tao, Yi, Qi-Bin, Yi, Shu-Xu, Yin, Qian-Qing, You, Yuan, Yu, Yun-Wei, Yu, Wei, Yu, Wen-Hui, Zeng, Ming, Zhang, Bing, Zhang, Bin-Bin, Zhang, Da-Li, Zhang, Fan, Zhang, Hong-Mei, Zhang, Juan, Zhang, Liang, Zhang, Peng, Zhang, Shu, Zhang, Shuang-Nan, Zhang, Wan-Chang, Zhang, Xiao-Feng, Zhang, Xiao-Lu, Zhang, Yan-Qiu, Zhang, Yan-Ting, Zhang, Yi-Fei, Zhang, Yuan-Hang, Zhang, Zhen, Zhao, Guo-Ying, Zhao, Hai-Sheng, Zhao, Hong-Yu, Zhao, Qing-Xia, Zhao, Shu-Jie, Zhao, Xiao-Yun, Zhao, Xiao-Fan, Zhao, Yi, Zheng, Chao, Zheng, Shi-Jie, Zhou, Deng-Ke, Zhou, Xing, and Zhu, Xiao-Cheng

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

GRB 221009A is the brightest gamma-ray burst ever detected since the discovery of this kind of energetic explosions. However, an accurate measurement of the prompt emission properties of this burst is very challenging due to its exceptional brightness. With joint observations of \textit{Insight}-HXMT and GECAM-C, we made an unprecedentedly accurate measurement of the emission during the first $\sim$1800 s of GRB 221009A, including its precursor, main emission (ME, which dominates the burst in flux), flaring emission and early afterglow, in the hard X-ray to soft gamma-ray band from $\sim$ 10 keV to $\sim$ 6 MeV. Based on the GECAM-C unsaturated data of the ME, we measure a record-breaking isotropic equivalent energy ($E_{\rm iso}$) of $\bf \sim 1.5 \times 10^{55}$ erg, which is about eight times the total rest-mass energy of the Sun. The early afterglow data require a significant jet break between 650 s and 1100 s, most likely at $\sim950$ s from the afterglow starting time $T_{AG}$, which corresponds to a jet opening angle of $\sim {0.7^\circ} \ (\eta_\gamma n)^{1/8}$, where $n$ is the ambient medium density in units of $\rm cm^{-3}$ and $\eta_\gamma$ is the ratio between $\gamma$-ray energy and afterglow kinetic energy. The beaming-corrected total $\gamma$-ray energy $E_{\gamma}$ is $\sim 1.15 \times10^{51} \ (\eta_\gamma n)^{1/4}$ erg, which is typical for long GRBs. These results suggest that this GRB may have a special central engine, which could launch and collimate a very narrowly beamed jet with an ordinary energy budget, leading to exceptionally luminous gamma-ray radiation per unit solid angle. Alternatively, more GRBs might have such a narrow and bright beam, which are missed by an unfavorable viewing angle or have been detected without distance measurement., Comment: Submitted to National Science Review. This paper is under press embargo, contact the corresponding author for details

Published
2023

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

Author

Liu, He-Xin, Huang, Yue, Xiao, Guang-Cheng, Bu, Qing-Cui, Qu, Jin-Lu, Zhang, Shu, Zhang, Shuang-Nan, Jia, Shu-Mei, Lu, Fang-Jun, Ma, Xiang, Tao, Lian, Zhang, Wei, Chen, Li, Song, Li-Ming, Li, Ti-Pei, Xu, Yu-Peng, Cao, Xue-Lei, Chen, Yong, Liu, Cong-Zhan, Cai, Ce, Chang, Zhi, Chen, Gang, Chen, Tian-Xiang, Chen, Yi-Bao, Chen, Yu-Peng, Cui, Wei, Cui, Wei-Wei, Deng, Jing-Kang, Dong, Yong-Wei, Du, Yuan-Yuan, Fu, Min-Xue, Gao, Guan-Hua, Gao, He, Gao, Min, Ge, Ming-Yu, Gu, Yu-Dong, Guan, Ju, Guo, Cheng-Cheng, Han, Da-Wei, Huo, Jia, Jiang, Lu-Hua, Jiang, Wei-Chun, Jin, Jing, Jin, Yong-Jie, Kong, Ling-Da, Li, Bing, Li, Cheng-Kui, Li, Gang, Li, Mao-Shun, Li, Wei, Li, Xian, Li, Xiao-Bo, Li, Xu-Fang, Li, Yang-Guo, Li, Zheng-Wei, Liang, Xiao-Hua, Liao, Jing-Yuan, Liu, Bai-Sheng, Liu, Guo-Qing, Liu, Hong-Wei, Liu, Xiao-Jing, Liu, Yi-Nong, Lu, Bo, Lu, Xue-Feng, Luo, Qi, Luo, Tao, Meng, Bin, Nang, Yi, Nie, Jian-Yin, Ou, Ge, Sai, Na, Shang, Ren-Cheng, Song, Xin-Ying, Sun, Liang, Tan, Ying, Tuo, You-Li, Wang, Chen, Wang, Guo-Feng, Wang, Juan, Wang, Ling-Jun, Wang, Weng-Shuai, Wang, Yu-Sa., Wen, Xiang-Yang, Wu, Bai-Yang, Wu, Bo-Bing, Wu, Mei, Xiao, Shuo, Xiong, Shao-Lin, Xu, He, Yang, Jia-Wei, Yang, Sheng, Yang, Yan-Ji, Yang, Yi-Jung, Yi, Qi-Bin, Yin, Qian-Qing, You, Yuan, Zhang, Ai-Mei, Zhang, Cheng-Mo, Zhang, Fan, Zhang, Hong-Mei, Zhang, Juan, Zhang, Tong, Zhang, Wan-Chang, Zhang, Wen-Zhao, Yi-Zhang, Zhang, Yi-Fei, Zhang, Yong-Jie, Zhang, Yuan-Hang, Zhang, Yue, Zhang, Zhao, Zhang, Zhi, Zhang, Zi-Liang, Zhao, Hai-Sheng, Zhao, Xiao-Fan, Zheng, Shi-Jie, Zheng, Yao-Guang, Zhou, Deng-Ke, Zhou, Jian-Feng, Zhu, Yu-Xuan, Zhuang, Ren-Lin, and Zhu, Yue

Subjects
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 classfied roughly into four different states. Type-C quasi-periodic oscillations (QPOs) observed by NICER (about 0.1-6Hz) and Insight-HXMT (about 0.7-8Hz) are also reported in this work. Meanwhile, we study various physical quantities related to QPO frequency.The QPO rms-frequency relationship in three 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
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8. Discovery of oscillations above 200 keV in a black hole X-ray binary with Insight-HXMT

Author

Ma, Xiang, Tao, Lian, Zhang, Shuang-Nan, Zhang, Liang, Bu, Qing-Cui, Ge, Ming-Yu, Chen, Yu-Peng, Qu, Jin-Lu, Zhang, Shu, Lu, Fang-Jun, Song, Li-Ming, Yang, Yi-Jung, Yuan, Feng, Cai, Ce, Cao, Xue-Lei, Chang, Zhi, Chen, Gang, Chen, Li, Chen, Tian-Xiang, Chen, Yi-Bao, Chen, Yong, Cui, Wei, Cui, Wei-Wei, Deng, Jing-Kang, Dong, Yong-Wei, Du, Yuan-Yuan, Fu, Min-Xue, Gao, Guan-Hua, Gao, He, Gao, Min, Gu, Yu-Dong, Guan, Ju, Guo, Cheng-Cheng, Han, Da-Wei, Huang, Yue, Huo, Jia, Ji, Long, Jia, Shu-Mei, Jiang, Lu-Hua, Jiang, Wei-Chun, Jin, Jing, Jin, Yong-Jie, Kong, Ling-Da, Li, Bing, Li, Cheng-Kui, Li, Gang, Li, Mao-Shun, Li, Ti-Pei, Li, Wei, Li, Xian, Li, Xiao-Bo, Li, Xu-Fang, Li, Yan-Guo, Li, Zheng-Wei, Liang, Xiao-Hua, Liao, Jin-Yuan, Liu, Bai-Sheng, Liu, Cong-Zhan, Liu, Guo-Qing, Liu, Hong-Wei, Liu, Xiao-Jing, Liu, Yi-Nong, Lu, Bo, Lu, Xue-Feng, Luo, Qi, Luo, Tao, Meng, Bin, Nang, Yi, Nie, Jian-Yin, Ou, Ge, Sai, Na, Shang, Ren-Cheng, Song, Xin-Ying, Sun, Liang, Tan, Ying, Tuo, Yuo-Li, Wang, Chen, Wang, Guo-Feng, Wang, Juan, Wang, Ling-Jun, Wang, Wen-Shuai, Wang, Yu-Sa, Wen, Xiang-Yang, Wu, Bai-Yang, Wu, Bo-Bing, Wu, Mei, Xiao, Guang-Cheng, Xiao, Shuo, Xie, Fu-Guo, Xiong, Shao-Lin, Xu, He, Xu, Yu-Peng, Yang, Jia-Wei, Yang, Sheng, Yang, Yan-Ji, Yi, Qi-Bin, Yin, Qian-Qing, You, Yuan, Zhang, Ai-Mei, Zhang, Cheng-Mo, Zhang, Fan, Zhang, Hong-Mei, Zhang, Juan, Zhang, Tong, Zhang, Wan-Chang, Zhang, Wei, Zhang, Wen-Zhao, Zhang, Yi, Zhang, Yi-Fei, Zhang, Yong-Jie, Zhang, Yue, Zhang, Zhao, Zhang, Zhi, Zhang, Zi-Liang, Zhao, Hai-Sheng, Zhao, Xiao-Fan, Zheng, Shi-Jie, Zhou, Deng-Ke, Zhou, Jian-Feng, Zhu, Yu-Xuan, Zhu, Yue, and Zhuang, Ren-Lin

Subjects
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., Comment: 36 pages, 12 figures, 3 tables; published in Nature Astronomy

Published
2020
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9. The influence of the Insight-HXMT/LE time response on timing analysis

Author

Zhou, Deng-Ke, Zheng, Shi-Jie, Song, Li-Ming, Chen, Yong, Li, Cheng-Kui, Li, Xiao-Bo, Chen, Tian-Xiang, Cui, Wei-Wei, Chen, Wei, Han, Da-Wei, Hu, Wei, Huo, Jia, Ma, Rui-Can, Li, Mao-Shun, Li, Tian-Ming, Li, Wei, Liu, He-Xin, Lu, Bo, Lu, Fang-Jun, Qu, Jin-Lu, Tuo, You-Li, Wang, Juan, Wang, Yu-Sa, Wu, Bai-Yang, Xiao, Guang-Cheng, Xu, Yu-Peng, Yang, Yan-Ji, Zhang, Shu, Zhang, Zi-Liang, Zhao, Xiao-Fan, and Zhu, Yu-Xuan

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
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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10. Studies on the time response distribution of Insigh}-HXMT/LE

Author

Zhao, Xiao-Fan, Zhu, Yu-Xuan, Han, Da-Wei, Cui, Wei-Wei, Li, Wei, Wang, Juan, Wang, Yu-Sa, Zhang, Yi, Yang, Yan-Ji, Lu, Bo, Huo, Jia, Zhang, Zi-Liang, Chen, Tian-Xiang, Li, Mao-Shun, Lv, Zhong-Hua, Chen, Yong, Bu, Qing-Cui, Cai, Ce, Cao, Xue-Lei, Chang, Zhi, Chen, Gang, Chen, Li, Chen, Yi-Bao, Chen, Yu-Peng, Cui, Wei, Deng, Jing-Kang, Dong, Yong-Wei, Du, Yuan-Yuan, Fu, Min-Xue, Gao, Guan-Hua, Gao, He, Gao, Min, Ge, Ming-Yu, Gu, Yu-Dong, Guan, Ju, Guo, Cheng-Cheng, Huang, Yue, Jia, Shu-Mei, Jiang, Lu-Hua, Jiang, Wei-Chun, Jin, Jing, Kong, Ling-Da, Li, Bing, Li, Cheng-Kui, Li, Gang, Li, Ti-Bei, Li, Xian, Li, Xiao-Bo, Li, Xu-Fang, Li, Yan-Guo, Li, Zheng-Wei, Liang, Xiao-Hua, Liao, Jin-Yuan, Liu, Cong-Zhan, Liu, Guo-Qing, Liu, Hong-Wei, Liu, Xiao-Jing, Liu, Yi-Nong, Lu, Fang-Jun, Lu, Xue-Feng, Luo, Qi, Luo, Tao, Ma, Xiang, Meng, Bin, Nang, Yi, Nie, Jian-Ying, Qu, Jin-Lu, Sai, Na, Song, Li-Ming, Song, Xin-Ying, Sun, Liang, Tan, Ying, Tao, Lian, Tuo, You-Li, Wang, Chen, Wang, Guo-Feng, Wen, Xiang-Yang, Wu, Bai-Yang, Wu, Bo-Bing, Wu, Mei, Xiao, Guang-Cheng, Xiao, Shuo, Xiong, Shao-Lin, Xu, Yu-Peng, Yang, Jia-Wei, Yang, Sheng, Yi, Qi-Bin, Yin, Qian-Qing, You, Yuan, Zhang, Ai-Mei, Zhang, Cheng-Mo, Zhang, Fan, Zhang, Juan, Zhang, Shu, Zhang, Shuang-Nan, Zhang, Tong, Zhang, Wan-Chang, Zhang, Wei, Zhang, Wen-Zhao, Zhang, Yi-Fei, Zhang, Yong-Jie, Zhang, Yue, Zhang, Zhao, Zhao, Hai-Sheng, Zheng, Shi-Jie, Zhou, Deng-Ke, Zhou, Jian-Feng, and Zhu, Yue

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Hard X-ray Modulation Telescope (HXMT) named Insight is China's first X-ray astronomical satellite. The Low Energy X-ray Telescope (LE) is one of its main payloads onboard. The detectors of LE adopt swept charge device CCD236 with L-shaped transfer electrodes. Charges in detection area are read out continuously along specific paths, which leads to a time response distribution of photons readout time. We designed a long exposure readout mode to measure the time response distribution. In this mode, CCD236 firstly performs exposure without readout, then all charges generated in preceding exposure phase are read out completely. Through analysis of the photons readout time in this mode, we obtained the probability distribution of photons readout time.

Published
2019

13. Confirming the spin parameter of the black hole in Cygnus X-1 using the Insight-HXMT

Author

Zhao, Xue-Shan, Dong, Yan-Ting, Gou, Li-Jun, Feng, Ye, Jia, Nan, Li, Yu-Feng, Liao, Zhen-Xuan, Liu, Ji-Ren, Zheng, Xue-Ying, Zhang, Shuang-Nan, Qu, Jin-Lu, Song, Li-Ming, Zhang, Shu, Bu, Qing-Cui, Cai, Ce, Cao, Xue-Lei, Chang, Zhi, Chen, Gang, Chen, Li, Chen, Tian-Xiang, Chen, Yi-Bao, Chen, Yong, Chen, Yu-Peng, Cui, Wei, Cui, Wei-Wei, Deng, Jing-Kang, Dong, Yong-Wei, Du, Yuan-Yuan, Fu, Min-Xue, Gao, Guan-Hua, Gao, He, Gao, Min, Ge, Ming-Yu, Gu, Yu-Dong, Guan, Ju, Guo, Cheng-Cheng, Han, Da-Wei, Huang, Yue, Huo, Jia, Jia, Shu-Mei, Jiang, Lu-Hua, Jiang, Wei-Chun, Jin, Jing, Jin, Yong-Jie, Kong, Ling-Da, Li, Bing, Li, Cheng-Kui, Li, Gang, Li, Mao-Shun, Li, Ti-Pei, Li, Wei, Li, Xian, Li, Xiao-Bo, Li, Xu-Fang, Li, Yan-Guo, Li, Zheng-Wei, Liang, Xiao-Hua, Liao, Jin-Yuan, Liu, Bai-Sheng, Liu, Cong-Zhan, Liu, Guo-Qing, Liu, He-Xin, Liu, Hong-Wei, Liu, Xiao-Jing, Liu, Yi-Nong, Lu, Bo, Lu, Fang-Jun, Lu, Xue-Feng, Luo, Qi, Luo, Tao, Ma, Xiang, Meng, Bin, Nang, Yi, Nie, Jian-Yin, Ou, Ge, Sai, Na, Shang, Ren-Cheng, Song, Xin-Ying, Sun, Liang, Tan, Ying, Tao, Lian, Tuo, You-Li, Wang, Chen, Wang, Guo-Feng, Wang, Juan, Wang, Wen-Shuai, Wang, Yu-Sa, Wen, Xiang-Yang, Wu, Bai-Yang, Wu, Bo-Bing, Wu, Mei, Xiao, Guang-Cheng, Xiao, Shuo, Xiong, Shao-Lin, Xu, Yu-Peng, Yang, Jia-Wei, Yang, Sheng, Yang, Yan-Ji, Yang, Yi-Rong, Yi, Qi-Bin, Yin, Qian-Qing, You, Yuan, Zhang, Ai-Mei, Zhang, Cheng-Mo, Zhang, Fan, Zhang, Hong-Mei, Zhang, Juan, Zhang, Tong, Zhang, Wan-Chang, Zhang, Wei, Zhang, Wen-Zhao, Zhang, Yi, Zhang, Yi-Fei, Zhang, Yong-Jie, Zhang, Yue, Zhang, Zhao, Zhang, Zhi, Zhang, Zi-Liang, Zhao, Hai-Sheng, Zhao, Xiao-Fan, Zheng, Shi-Jie, Zhou, Deng-Ke, Zhou, Jian-Feng, Zhu, Yu-Xuan, Yue-Zhu, and Zhuang, Ren-Lin

Published
2020
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15. A digital CDS technique and the performance testing

Author

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

Subjects
Physics - Instrumentation and Detectors, Nuclear Experiment
Abstract

Readout noise is a critical parameter for characterizing the performance of charge-coupled devices (CCDs), which can be greatly reduced by the correlated double sampling (CDS) circuit. However, conventional CDS circuit inevitably introduces new noises since it consists of several active analog components such as operational amplifiers. This paper proposes a digital CDS circuit technique, which transforms the pre-amplified CCD signal into a train of digital presentations by a high-speed data acquisition card directly without the noisy CDS circuit first, then implement the digital CDS algorithm through numerical method. The readout noise of 3.3 e$^{-}$ and the energy resolution of 121 eV@5.9keV can be achieved via the digital CDS technique.

Published
2014

16. Proton irradiation effect on SCDs

Author

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

Subjects
Physics - Instrumentation and Detectors, Nuclear Experiment
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 digital CDS technique and its performance testing

Author

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

Subjects
Synchrotrons and Accelerators, Physical Sciences, physics.ins-det, nucl-ex, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Atomic, molecular and optical physics, Particle and high energy physics
Abstract

Readout noise is a critical parameter for characterizing the performance of charge-coupled devices (CCDs), which can be greatly reduced by the correlated double sampling (CDS) circuit. However, a conventional CDS circuit inevitably introduces new noise since it consists of several active analog components such as operational amplifiers. This paper proposes a digital CDS circuit technique, which transforms the pre-amplified CCD signal into a train of digital presentations by a high-speed data acquisition card directly without the noisy CDS circuit, then implements the digital CDS algorithm through a numerical method. A readout noise of 3.3 e- and an energy resolution of 121 eV@5.9 keV can be achieved via the digital CDS technique.

Published
2015

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

Author

Liu, He-Xin, primary, Huang, Yue, additional, Xiao, Guang-Cheng, additional, Bu, Qing-Cui, additional, Qu, Jin-Lu, additional, Zhang, Shu, additional, Zhang, Shuang-Nan, additional, Jia, Shu-Mei, additional, Lu, Fang-Jun, additional, Ma, Xiang, additional, Tao, Lian, additional, Zhang, Wei, additional, Chen, Li, additional, Song, Li-Ming, additional, Li, Ti-Pei, additional, Xu, Yu-Peng, additional, Cao, Xue-Lei, additional, Chen, Yong, additional, Liu, Cong-Zhan, additional, Cai, Ce, additional, Chang, Zhi, additional, Chen, Gang, additional, Chen, Tian-Xiang, additional, Chen, Yi-Bao, additional, Chen, Yu-Peng, additional, Cui, Wei, additional, Cui, Wei-Wei, additional, Deng, Jing-Kang, additional, Dong, Yong-Wei, additional, Du, Yuan-Yuan, additional, Fu, Min-Xue, additional, Gao, Guan-Hua, additional, Gao, He, additional, Gao, Min, additional, Ge, Ming-Yu, additional, Gu, Yu-Dong, additional, Guan, Ju, additional, Guo, Cheng-Cheng, additional, Han, Da-Wei, additional, Huo, Jia, additional, Jiang, Lu-Hua, additional, Jiang, Wei-Chun, additional, Jin, Jing, additional, Jin, Yong-Jie, additional, Kong, Ling-Da, additional, Li, Bing, additional, Li, Cheng-Kui, additional, Li, Gang, additional, Li, Mao-Shun, additional, Li, Wei, additional, Li, Xian, additional, Li, Xiao-Bo, additional, Li, Xu-Fang, additional, Li, Yang-Guo, additional, Li, Zheng-Wei, additional, Liang, Xiao-Hua, additional, Liao, Jing-Yuan, additional, Liu, Bai-Sheng, additional, Liu, Guo-Qing, additional, Liu, Hong-Wei, additional, Liu, Xiao-Jing, additional, Liu, Yi-Nong, additional, Lu, Bo, additional, Lu, Xue-Feng, additional, Luo, Qi, additional, Luo, Tao, additional, Meng, Bin, additional, Nang, Yi, additional, Nie, Jian-Yin, additional, Ou, Ge, additional, Sai, Na, additional, Shang, Ren-Cheng, additional, Song, Xin-Ying, additional, Sun, Liang, additional, Tan, Ying, additional, Tuo, You-Li, additional, Wang, Chen, additional, Wang, Guo-Feng, additional, Wang, Juan, additional, Wang, Ling-Jun, additional, Wang, Weng-Shuai, additional, Wang, Yu-Sa, additional, Wen, Xiang-Yang, additional, Wu, Bai-Yang, additional, Wu, Bo-Bing, additional, Wu, Mei, additional, Xiao, Shuo, additional, Xiong, Shao-Lin, additional, Xu, He, additional, Yang, Jia-Wei, additional, Yang, Sheng, additional, Yang, Yan-Ji, additional, Yang, Yi-Jung, additional, Yi, Qi-Bin, additional, Yin, Qian-Qing, additional, You, Yuan, additional, Zhang, Ai-Mei, additional, Zhang, Cheng-Mo, additional, Zhang, Fan, additional, Zhang, Hong-Mei, additional, Zhang, Juan, additional, Zhang, Tong, additional, Zhang, Wan-Chang, additional, Zhang, Wen-Zhao, additional, Zhang, Yi, additional, Zhang, Yi-Fei, additional, Zhang, Yong-Jie, additional, Zhang, Yuan-Hang, additional, Zhang, Yue, additional, Zhang, Zhao, additional, Zhang, Zhi, additional, Zhang, Zi-Liang, additional, Zhao, Hai-Sheng, additional, Zhao, Xiao-Fan, additional, Zheng, Shi-Jie, additional, Zheng, Yao-Guang, additional, Zhou, Deng-Ke, additional, Zhou, Jian-Feng, additional, Zhu, Yu-Xuan, additional, Zhuang, Ren-Lin, additional, and Zhu, Yue, additional

Published
2021
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31. The influence of the Insight-HXMT/LE time response on timing analysis

Author

Zhou, Deng-Ke, primary, Zheng, Shi-Jie, additional, Song, Li-Ming, additional, Chen, Yong, additional, Li, Cheng-Kui, additional, Li, Xiao-Bo, additional, Chen, Tian-Xiang, additional, Cui, Wei-Wei, additional, Chen, Wei, additional, Han, Da-Wei, additional, Hu, Wei, additional, Huo, Jia, additional, Ma, Rui-Can, additional, Li, Mao-Shun, additional, Li, Tian-Ming, additional, Li, Wei, additional, Liu, He-Xin, additional, Lu, Bo, additional, Lu, Fang-Jun, additional, Qu, Jin-Lu, additional, Tuo, You-Li, additional, Wang, Juan, additional, Wang, Yu-Sa, additional, Wu, Bai-Yang, additional, Xiao, Guang-Cheng, additional, Xu, Yu-Peng, additional, Yang, Yan-Ji, additional, Zhang, Shu, additional, Zhang, Zi-Liang, additional, Zhao, Xiao-Fan, additional, and Zhu, Yu-Xuan, additional

Published
2021
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32. Discovery of oscillations above 200 keV in a black hole X-ray binary with Insight-HXMT

Author

Ma, Xiang, primary, Tao, Lian, additional, Zhang, Shuang-Nan, additional, Zhang, Liang, additional, Bu, Qing-Cui, additional, Ge, Ming-Yu, additional, Chen, Yu-Peng, additional, Qu, Jin-Lu, additional, Zhang, Shu, additional, Lu, Fang-Jun, additional, Song, Li-Ming, additional, Yang, Yi-Jung, additional, Yuan, Feng, additional, Cai, Ce, additional, Cao, Xue-Lei, additional, Chang, Zhi, additional, Chen, Gang, additional, Chen, Li, additional, Chen, Tian-Xiang, additional, Chen, Yi-Bao, additional, Chen, Yong, additional, Cui, Wei, additional, Cui, Wei-Wei, additional, Deng, Jing-Kang, additional, Dong, Yong-Wei, additional, Du, Yuan-Yuan, additional, Fu, Min-Xue, additional, Gao, Guan-Hua, additional, Gao, He, additional, Gao, Min, additional, Gu, Yu-Dong, additional, Guan, Ju, additional, Guo, Cheng-Cheng, additional, Han, Da-Wei, additional, Huang, Yue, additional, Huo, Jia, additional, Ji, Long, additional, Jia, Shu-Mei, additional, Jiang, Lu-Hua, additional, Jiang, Wei-Chun, additional, Jin, Jing, additional, Jin, Yong-Jie, additional, Kong, Ling-Da, additional, Li, Bing, additional, Li, Cheng-Kui, additional, Li, Gang, additional, Li, Mao-Shun, additional, Li, Ti-Pei, additional, Li, Wei, additional, Li, Xian, additional, Li, Xiao-Bo, additional, Li, Xu-Fang, additional, Li, Yan-Guo, additional, Li, Zheng-Wei, additional, Liang, Xiao-Hua, additional, Liao, Jin-Yuan, additional, Liu, Bai-Sheng, additional, Liu, Cong-Zhan, additional, Liu, Guo-Qing, additional, Liu, Hong-Wei, additional, Liu, Xiao-Jing, additional, Liu, Yi-Nong, additional, Lu, Bo, additional, Lu, Xue-Feng, additional, Luo, Qi, additional, Luo, Tao, additional, Meng, Bin, additional, Nang, Yi, additional, Nie, Jian-Yin, additional, Ou, Ge, additional, Sai, Na, additional, Shang, Ren-Cheng, additional, Song, Xin-Ying, additional, Sun, Liang, additional, Tan, Ying, additional, Tuo, Yuo-Li, additional, Wang, Chen, additional, Wang, Guo-Feng, additional, Wang, Juan, additional, Wang, Ling-Jun, additional, Wang, Wen-Shuai, additional, Wang, Yu-Sa, additional, Wen, Xiang-Yang, additional, Wu, Bai-Yang, additional, Wu, Bo-Bing, additional, Wu, Mei, additional, Xiao, Guang-Cheng, additional, Xiao, Shuo, additional, Xie, Fu-Guo, additional, Xiong, Shao-Lin, additional, Xu, He, additional, Xu, Yu-Peng, additional, Yang, Jia-Wei, additional, Yang, Sheng, additional, Yang, Yan-Ji, additional, Yi, Qi-Bin, additional, Yin, Qian-Qing, additional, You, Yuan, additional, Zhang, Ai-Mei, additional, Zhang, Cheng-Mo, additional, Zhang, Fan, additional, Zhang, Hong-Mei, additional, Zhang, Juan, additional, Zhang, Tong, additional, Zhang, Wan-Chang, additional, Zhang, Wei, additional, Zhang, Wen-Zhao, additional, Zhang, Yi, additional, Zhang, Yi-Fei, additional, Zhang, Yong-Jie, additional, Zhang, Yue, additional, Zhang, Zhao, additional, Zhang, Zhi, additional, Zhang, Zi-Liang, additional, Zhao, Hai-Sheng, additional, Zhao, Xiao-Fan, additional, Zheng, Shi-Jie, additional, Zhou, Deng-Ke, additional, Zhou, Jian-Feng, additional, Zhu, Yu-Xuan, additional, Zhu, Yue, additional, and Zhuang, Ren-Lin, additional

Published
2020
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35. Microstructural Configuration and Impact Toughness of Graphite Ductile Iron Reinforced by Trace Amount of TiC-TiB2 Nanoparticles.

Author

Cui, Wei-Wei, Wang, Bing-Xu, Qiu, Feng, Zhang, Yu, Yang, Jing, Zhang, Zhaoxia, Barber, Gary C., and Hu, Ming

Subjects
NODULAR iron, GRAPHITE, NANOPARTICLES, DUCTILE fractures, ALUMINUM alloys, IRON alloys, IRON composites
Abstract

The present research investigated the effects of TiC-TiB2 nanoparticles on the microstructure and impact toughness of graphite ductile iron. The nanoparticle-reinforced ductile iron samples were prepared by using an aluminum master alloy containing TiC-TiB2 nanoparticles. It was found that the addition of nanoparticles refined the graphite nodules, pearlitic structure and grains. According to the edge-to-edge matching model, the nanoparticles served as nucleation sites for graphite and austenite during the liquid-solid phase transformation. Moreover, the impact toughness was improved by 50.4, 36.2 and 28.3% at the temperatures of 20, 0 and − 20 °C. The fracture surfaces were dominated by cleavage fracture for ductile iron without nanoparticles. After adding nanoparticles, ductile risers were found around graphite nodules, and some nanoparticles were detected within the dimples on the ductile risers. [ABSTRACT FROM AUTHOR]

Published
2022
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36. Hard X-ray imaging based on CCD and CsI scintillator

Author

陈勇 Chen Yong, 陆波 Lu Bo, 杨彦佶 Yang Yan-ji, 王于仨 Wang Yu-sa, and 崔苇苇 Cui Wei-wei

Subjects
Physics, Optics, 010308 nuclear & particles physics, business.industry, 0103 physical sciences, X-ray, Scintillator, 010306 general physics, business, 01 natural sciences, Atomic and Molecular Physics, and Optics, Electronic, Optical and Magnetic Materials
Published
2017
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38. Studies on the time response distribution of Insight-HXMT/LE

Author

Zhao, Xiao-Fan, primary, Zhu, Yu-Xuan, additional, Han, Da-Wei, additional, Cui, Wei-Wei, additional, Li, Wei, additional, Wang, Juan, additional, Wang, Yu-Sa, additional, Zhang, Yi, additional, Yang, Yan-Ji, additional, Lu, Bo, additional, Huo, Jia, additional, Zhang, Zi-Liang, additional, Chen, Tian-Xiang, additional, Li, Mao-Shun, additional, Lv, Zhong-Hua, additional, and Chen, Yong, additional

Published
2019
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39. Low temperature testing and neutron irradiation of a swept charge device on board the HXMT satellite

Author

Zhu Yue, Li Wei, Yang Yan-Ji, Huo Jia, Cui Wei-Wei, Liu Xiaoyan, Han Da-Wei, L. T. Yan, Li Maoshun, Zhang Zi-Liang, Chen Yong, Wu Di, Li Zheng-Wei, Lu Bo, Hu Wei, Sun Qing-Rong, Chen Tian-Xiang, Zhang Yi, Wang Juan, Xu Yu-Peng, Wang Yu-Sa, and Li Cheng-Kui

Subjects
Physics, Nuclear and High Energy Physics, Physics::Instrumentation and Detectors, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Resolution (electron density), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Atmospheric temperature range, Fluence, Full width at half maximum, Optics, Satellite, business, Instrumentation, Noise (radio), Dark current
Abstract

We present the low temperature testing of an SCD detector, investigating its performance such as readout noise, energy resolution at 5.9 keV and dark current. The SCD's performance is closely related to temperature, and the temperature range of −80 °C to −50 °C is the best choice, where the FWHM at 5.9 keV is about 130 eV. The influence of the neutron irradiation from an electrostatic accelerator with fluence up to 1 × 109 cm−2 has been examined. We find the SCD is not vulnerable to neutron irradiation. The detailed operations of the SCD and the test results of low temperature are reported, and the results of neutron irradiation are discussed.

Published
2012
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40. Design and optimization of the readout system for X-ray CCDs

Author

Li Wei, Cui Wei-Wei, Lu Bo, Chen Yong, Han Da-Wei, Li Cheng-Kui, Huo Jia, Li Maoshun, Zhang Yi, Chen Tian-Xiang, Zhu Yue, Wang Yu-Sa, Liu Xiaoyan, Wang Juan, Xu Yu-Peng, Yang Yan-Ji, and Hu Wei

Subjects
Physics, Nuclear and High Energy Physics, Pixel, Physics::Instrumentation and Detectors, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, X-ray, Astronomy and Astrophysics, Noise (electronics), Full width at half maximum, Analog signal, Optics, business, Instrumentation
Abstract

A readout system for X-ray CCDs based on an improved architecture is presented; by optimizing several critical circuit blocks along the analog signal chain, the conflict between the readout speed and readout noise is greatly alleviated. Using CCD47-10 as its target CCD, the readout system has achieved 8.6e− readout noise and 142 eV FWHM at 5.9 keV Mn Kα under a pixel rate of 80 kHz. Also its performance of imaging has been investigated.

Published
2012
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41. A digital CDS technique and its performance testing**Supported by National Natural Science Foundation of China (10978002)

Author

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

Subjects
Particle and Plasma Physics, Molecular, Nuclear, nucl-ex, physics.ins-det, Atomic, Nuclear & Particles Physics
Abstract

Readout noise is a critical parameter for characterizing the performance of charge-coupled devices (CCDs), which can be greatly reduced by the correlated double sampling (CDS) circuit. However, a conventional CDS circuit inevitably introduces new noise since it consists of several active analog components such as operational amplifiers. This paper proposes a digital CDS circuit technique, which transforms the pre-amplified CCD signal into a train of digital presentations by a high-speed data acquisition card directly without the noisy CDS circuit, then implements the digital CDS algorithm through a numerical method. A readout noise of 3.3 e- and an energy resolution of 121 eV@5.9 keV can be achieved via the digital CDS technique.

Published
2015

42. Reducing Error in Mail Surveys

Author

Cui, Wei Wei

Subjects
Questionnaires, lcsh:Theory and practice of education, Survey Research, Research Design, Responses, Research Methodology, lcsh:LB5-3640, Mail Surveys, Response Rates
Abstract

Surveys allow information to be collected from a sample group and generalized to the population at large. Because they are low cost and easy to implement, mail surveys are used more frequently for social research than either telephone or face-to-face interviews. Those conducting surveys should recognize four potential sources of error -- sampling error, noncoverage error, non-response error, and measurement error -- and take steps to minimize their impact. Any one of these sources of error may make the survey results unacceptable (Groves, 1989; Salant and Dillman, 1994; Dillman, 1991, 1999). This article describes the four types of errors and summarizes ways they can be reduced. Accessed 65,275 times on https://pareonline.net from September 02, 2003 to December 31, 2019. For downloads from January 1, 2020 forward, please click on the PlumX Metrics link to the right.

Published
2003

44. Quantum efficiency calibration for low energy detector in hard X-ray modulation telescope satellite

Author

Xue Rongfeng, Yang Yan-Ji, Chen Yong, Zhao Xiao-Fan, Huo Jia, Zhang Yi, Lu Bo, Chen Tian-Xiang, Liu Miao, Wang Yu-Sa, Wang Juan, Zhang Zi-Liang, Han Da-Wei, Zhu-Yue, Li Wei, Li Maoshun, Cui Wei-Wei, Hu Wei, and Zhu Yu-Xuan

Subjects
Physics, Silicon drift detector, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Radioactive source, Detector, General Physics and Astronomy, law.invention, Luminosity, Telescope, Optics, Depletion region, law, Quantum efficiency, Charge-coupled device, business
Abstract

Low energy X-ray telescope, working over 0.7-15 keV energy band, is one of the main payloads in the hard X-ray modulation telescope satellite. The primary scientific objectives are to survey large sky area to investigate galactic X-ray transient sources as well as the cosmic X-ray background, and to observe X-ray binaries or black holes for studying the dynamics and emission mechanism in strong gravitational or magnetic field. The detector of low energy X-ray telescope is CCD236, a new generation of swept charge device, which has good time and energy resolution. Quantum efficiency (QE) of the detector has a crucial influence on X-ray spectrum fitting and absolute luminosity calculation. To provide valuable scientific data, QE should be calibrated in detail. In this paper, QE calibration is accomplished with respect to a silicon drift detector (SDD), using an Fe-55 radioactive source, at energy points Mn-K-alpha (5.899 keV) and Mn-K-beta (6.497 keV). The energies of Mn-K-alpha and Mn-K-beta are near that of iron-K, which is an important line in X-ray observation. Additionally, Mn-K-alpha and Mn-K-beta X-ray will partially pass through the depletion region of CCD236, and these energy points can be used to measure the depletion thickness. This experiment is set up in a vacuum cooling chamber. The X-ray source perpendicularly illuminates SDD and CCD236 through a small hole, whose area is far less than those of two detectors; therefore, QE measurements are irrelevant to neither the distance nor the azimuth angle between the X-ray source and the detector. For CCD236, split events should be corrected. Energy spectra of SDD and CCD236 are fitted with two Gaussian distributions, respectively, to obtain peak positions and standard variations of Mn-K-alpha and Mn-K-beta. With known structure of SDD, the QE of CCD236 can be calculated. QE values at Mn-K-alpha and Mn-K-beta are 71% and 62%, respectively. QE and temperature are uncorrelated with each other in a temperature range from -95 degrees C to -30 degrees C. According to the specific structure of CCD236 and the measured QE, without considering the effect of channel stop, the best-fit thickness of depletion region is obtained to be 38 mu m. When CCD236 is applied with different driving or substrate voltages, no obvious variation of QE is observed. It indicates that the thickness values of depletion region with high and low level voltages are equal. Furthermore, it shows that working CCD236 is deep depleted, and the thickness of depletion region will not change because it reaches its maximum, the edge of epitaxial layer and substrate layer.

Published
2017
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50. Proton irradiation effect on SCDs

Author

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

Published
2014
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