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41 results on '"Yang, Yan-Ji"'

1. 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

2. Five-year in-orbit background of Insight-HXMT

Author

Liao, Jin-Yuan, Zhang, Shu, Zhang, Juan, Li, Gang, Chang, Zhi, Chen, Yu-Peng, Ge, Ming-Yu, Jin, Jing, Lu, Xue-Feng, You, Yuan, Cao, Xue-Lei, Chen, Yong, Huang, Yue, Jiang, Wei-Chun, Li, Xiao-Bo, Li, Xu-Fang, Li, Zheng-Wei, Liu, Cong-Zhan, Tan, Ying, Yang, Yan-Ji, Zhang, Yi-Fei, Zhao, Hai-Sheng, Lu, Fang-Jun, Xu, Yu-Peng, Qu, Jin-Lu, Song, Li-Ming, and Zhang, Shuang-Nan

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Purpose: We present the five-year in-orbit background evolution of Insight-HXMT since the launch, as well as the effects of the background model in data analysis. Methods: The backgrounds of the three main payloads, i.e., Low-Energy Telescope, Medium-Energy Telescope and High-Energy Telescope, are described, respectively. The evolution of the background over time is obtained by simply comparing the background in every year during the in-orbit operation of Insight-HXMT. Results: The major observational characteristics of the Insight-HXMT in-orbit background are presented, including the light curve, spectrum, geographical distribution, and long-term evolution. The systematic error in background estimation is investigated for every year. Conclusion: The observational characteristics of the five-year in-orbit background are consistent with our knowledge of the satellite design and the space environment, and the background model is still valid for the latest observations of Insight-HXMT., Comment: 22 pages, 25 figures, accepted for publication in RDTM

Published
2023

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

Author

Wang, P. J., Kong, L. D., Zhang, S., Chen, Y. P., Zhang, S. N., Qu, J. L., Ji, L., Tao, L., Ge, M. Y., Lu, F. J., Chen, L., Song, L. M., Li, T. P., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Bu, Q. C., Cai, C., Chang, Z., Chen, G., Chen, T. X., Chen, Y. B., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, L. H., Jiang, W. C., Jin, J., Jin, Y. J., Li, B., Li, C. K., Li, G., Li, M. S., Li, W., Li, X., Li, X. B., Li, X. F., Li, Y. G., Li, Z. W., Liang, X. H., Liao, J. Y., Liu, B. S., Liu, G. Q., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, X. F., Luo, Q., Luo, T., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Sai, N., Shang, R. C., Song, X. Y., Sun, L., Tan, Y., Tuo, Y. L., Wang, C., Wang, G. F., Wang, J., Wang, L. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, J. W., Yang, S., Yang, Yan Ji, Yang, Yi Jung, Yi, Q. B., Yin, Q. Q., You, Y., Zhang, A. M., Zhang, C. M., Zhang, F., Zhang, H. M., Zhang, J., Zhang, T., Zhang, W. C., Zhang, W., Zhang, W. Z., Zhang, Y., Zhang, Y. F., Zhang, Y. J., Zhang, Zhao, Zhang, Zhi, Zhang, Z. L., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., Zhou, D. K., Zhou, J. F., Zhu, Y. X., Zhu, Y., and Zhuang, R. L.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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 source (ULX) 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 super-critical 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 $7.71\times10^{38}$~erg~s$^{-1}$, but smaller at above. A transition luminosity is found to be energy independent. Such a phenomena is firstly confirmed by Insight-HXMT observations and we speculate it may have relation with the radiation pressure dominated accretion disk.

Published
2020
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4. X-ray reprocessing in accreting pulsar GX 301-2 observed with Insight-HXMT

Author

Ji, L., Doroshenko, V., Suleimanov, V., Santangelo, A., Orlandini, M., Liu, J., Ducci, L., Zhang, S. N., Nabizadeh, A., Gavran, D., Zhang, S., Ge, M. Y., Li, X. B., Tao, L., Bu, Q. C., Qu, J. L., Lu, F. J., Chen, L., Song, L. M., Li, T. P., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Cai, C., Chang, Z., Chen, T. X., Chen, Y. P., Cui, W. W., Du, Y. Y., Gao, G. H., Gao, H., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, W. C., Jin, J., Kong, L. D., Li, B., Li, C. K., Li, G., Li, W., Li, X., Li, X. F., Li, Z. W., Liang, X. H., Liao, J. Y., Liu, B. S., Liu, H. X., Liu, H. W., Liu, X. J., Lu, X. F., Luo, Q., Luo, T., Ma, R. C., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Ren, X. Q., Sai, N., Song, X. Y., Sun, L., Tan, Y., Tuo, Y. L., Wang, C., Wang, L. J., Wang, P. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, R. J., Yang, S., Yang, Yan-Ji, Yang, Yi-Jung, Yi, Q. B., Yin, Q. Q., You, Y., Zhang, F., Zhang, H. M., Zhang, J., Zhang, P., Zhang, W., Zhang, W. C., Zhang, Yi, Zhang, Y. F., Zhang, Y. H., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., and Zhou, D. K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We investigate the absorption and emission features in observations of GX 301-2 detected with Insight-HXMT/LE in 2017-2019. At different orbital phases, we found prominent Fe Kalpha, Kbeta and Ni Kalpha lines, as well as Compton shoulders and Fe K-shell absorption edges. These features are due to the X-ray reprocessing caused by the interaction between the radiation from the source and surrounding accretion material. According to the ratio of iron lines Kalpha and Kbeta, we infer the accretion material is in a low ionisation state. We find an orbital-dependent local absorption column density, which has a large value and strong variability around the periastron. We explain its variability as a result of inhomogeneities of the accretion environment and/or instabilities of accretion processes. In addition, the variable local column density is correlated with the equivalent width of the iron Kalpha lines throughout the orbit, which suggests that the accretion material near the neutron star is spherically distributed., Comment: 10 pages, 5 figures, 2 tables, accepted for publication in MNRAS

Published
2020
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5. 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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6. 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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7. 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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8. Background Model for the Low-Energy Telescope of Insight-HXMT

Author

Liao, Jin-Yuan, Zhang, Shu, Chen, Yong, Zhang, Juan, Jin, Jing, Chang, Zhi, Chen, Yu-Peng, Ge, Ming-Yu, Guo, Cheng-Cheng, Li, Gang, Li, Xiao-Bo, Lu, Fang-Jun, Lu, Xue-Feng, Nie, Jian-Yin, Song, Li-Ming, Yang, Yan-Ji, You, Yuan, Zhao, Hai-Sheng, and Zhang, Shuang-Nan

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

With more than 150 blank sky observations at high Galactic latitude, we make a systematic study to the background of the Low Energy Telescope (LE) of the Hard X-ray Modulation Telescope (dubbed as Insight-HXMT). Both the on-ground simulation and the in-orbit observation indicate that the background spectrum mainly has two components. One is the particle background that dominates above 7 keV and its spectral shape is consistent in every geographical locations. Another is the diffuse X-ray background that dominates below 7 keV and has a stable spectrum less dependent of the sky region. The particle background spectral shape can be obtained from the blind detector data of all the blank sky observations, and the particle background intensity can be measured by the blind detector at 10-12.5 keV. The diffuse X-ray background in the high Galactic latitude can also be obtained from the blank sky spectra after subtracting the particle background. Based on these characteristics, we develop the background model for both the spectrum and the light curve. The systematic error for the background spectrum is investigated with different exposures (T_exp). For the spectrum with T_exp=1 ks, the average systematic errors in 1-7 keV and 1-10 keV are 4.2% and 3.7%, respectively. We also perform the systematic error analyses of the background light curves with different energy bands and time bins. The results show that the systematic errors for the light curves with different time bins are <8% in 1-10 keV., Comment: 24 pages, 17 figures, accepted by Journal of High Energy Astrophysics

Published
2020

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

Author

Ji, L., Ducci, L., Santangelo, A., Zhang, S., Suleimanov, V., Tsygankov, S., Doroshenko, V., Nabizadeh, A., Zhang, S. N., Ge, M. Y., Tao, L., Bu, Q. C., Qu, J. L., Lu, F. J., Chen, L., Song, L. M., Li, T. P., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Cai, C., Chang, Z., Chen, G., Chen, T. X., Chen, Y. B., Chen, Y. P., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, L. H., Jiang, W. C., Jin, J., Kong, L. D., Li, B., Li, C. K., Li, G., Li, M. S., Li, W., Li, X., Li, X. B., Li, X. F., Li, Y. G., Li, Z. W., Liang, X. H., Liao, J. Y., Liu, G. Q., Liu, H. X., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, X. F., Luo, Q., Luo, T., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Ren, X. Q., Sai, N., Song, X. Y., Sun, L., Tan, Y., Tuo, Y. L., Wang, C., Wang, G. F., Wang, J., Wang, P. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, J. W., Yang, S., Yang, Yan-Ji, Yang, Yi-Jung, Yi, Q. B., Yin, Q. Q., You, Y., Zhang, A. M., Zhang, C. M., Zhang, F., Zhang, H. M., Zhang, J., Zhang, P., Zhang, T., Zhang, W., Zhang, W. C., Zhang, W. Z., Zhang, Yi, Zhang, Y. F., Zhang, Y. J., Zhang, Y. H., Zhang, Yue, Zhang, Z., Zhang, Z. L., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zhou, D. K., Zhou, J. F., Zhu, Y. X., and Zhu, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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., Comment: 11 pages, 8 figures, accepted for publication in MNRAS

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

11. 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

12. 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

Published
2021
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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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14. 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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15. 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
physics.ins-det, nucl-ex, Atomic, Molecular, Nuclear, Particle and Plasma Physics, 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

16. Five-year in-orbit background of Insight-HXMT

Author

Liao, Jin-Yuan, primary, Zhang, Shu, additional, Zhang, Juan, additional, Li, Gang, additional, Chang, Zhi, additional, Chen, Yu-Peng, additional, Ge, Ming-Yu, additional, Jin, Jing, additional, Lu, Xue-Feng, additional, You, Yuan, additional, Cao, Xue-Lei, additional, Chen, Yong, additional, Huang, Yue, additional, Jiang, Wei-Chun, additional, Li, Xiao-Bo, additional, Li, Xu-Fang, additional, Li, Zheng-Wei, additional, Liu, Cong-Zhan, additional, Tan, Ying, additional, Yang, Yan-Ji, additional, Zhang, Yi-Fei, additional, Zhao, Hai-Sheng, additional, Lu, Fang-Jun, additional, Xu, Yu-Peng, additional, Qu, Jin-Lu, additional, Song, Li-Ming, additional, and Zhang, Shuang-Nan, additional

Published
2023
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18. The 2018 failed outburst of H 1743 – 322: Insight-HXMT, NuSTAR, and NICER views

Author

Wang, P J, primary, Kong, L D, additional, Chen, Y P, additional, Zhang, S, additional, Zhang, S N, additional, Soria, R, additional, Ji, L, additional, Qu, J L, additional, Huang, Y, additional, Tao, L, additional, Ge, M Y, additional, Lu, F J, additional, Chen, L, additional, Li, T P, additional, Xu, Y P, additional, Cao, X L, additional, Chen, Y, additional, Liu, C Z, additional, Bu, Q C, additional, Cai, C, additional, Chang, Z, additional, Chen, T X, additional, Chen, Y B, additional, Cui, W W, additional, Du, Y Y, additional, Gao, G H, additional, Gao, H, additional, Gu, Y D, additional, Guan, J, additional, Guo, C C, additional, Han, D W, additional, Huo, J, additional, Jia, S M, additional, Jiang, W C, additional, Jin, J, additional, Li, B, additional, Li, C K, additional, Li, G, additional, Li, W, additional, Li, X, additional, Li, X B, additional, Li, X F, additional, Li, Z W, additional, Liang, X H, additional, Liao, J Y, additional, Liu, B S, additional, Liu, H X, additional, Liu, H W, additional, Liu, X J, additional, Lu, X F, additional, Luo, Q, additional, Luo, T, additional, Ma, R C, additional, Ma, X, additional, Meng, B, additional, Nang, Y, additional, Nie, J Y, additional, Ou, G, additional, Ren, X Q, additional, Sai, N, additional, Song, L M, additional, Song, X Y, additional, Sun, L, additional, Tan, Y, additional, Tuo, Y L, additional, Wang, C, additional, Wang, L J, additional, Wang, W S, additional, Wang, Y S, additional, Wen, X Y, additional, Wu, B Y, additional, Wu, B B, additional, Wu, M, additional, Xiao, G C, additional, Xiao, S, additional, Xiong, S L, additional, Yang, R J, additional, Yang, S, additional, Yang, Yan Ji, additional, Yang, Yi Jung, additional, Yi, Q B, additional, Yin, Q Q, additional, You, Y, additional, Zhang, F, additional, Zhang, H M, additional, Zhang, J, additional, Zhang, P, additional, Zhang, W C, additional, Zhang, W, additional, Zhang, Y F, additional, Zhang, Y H, additional, Zhao, H S, additional, Zhao, X F, additional, Zheng, S J, additional, Zheng, Y G, additional, and Zhou, D K, additional

Published
2022
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19. 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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20. 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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21. X-ray reprocessing in accreting pulsar GX 301-2 observed with Insight-HXMT

Author

Ji, L, primary, Doroshenko, V, additional, Suleimanov, V, additional, Santangelo, A, additional, Orlandini, M, additional, Liu, J, additional, Ducci, L, additional, Zhang, S N, additional, Nabizadeh, A, additional, Gavran, D, additional, Zhang, S, additional, Ge, M Y, additional, Li, X B, additional, Tao, L, additional, Bu, Q C, additional, Qu, J L, additional, Lu, F J, additional, Chen, L, additional, Song, L M, additional, Li, T P, additional, Xu, Y P, additional, Cao, X L, additional, Chen, Y, additional, Liu, C Z, additional, Cai, C, additional, Chang, Z, additional, Chen, T X, additional, Chen, Y P, additional, Cui, W W, additional, Du, Y Y, additional, Gao, G H, additional, Gao, H, additional, Gu, Y D, additional, Guan, J, additional, Guo, C C, additional, Han, D W, additional, Huang, Y, additional, Huo, J, additional, Jia, S M, additional, Jiang, W C, additional, Jin, J, additional, Kong, L D, additional, Li, B, additional, Li, C K, additional, Li, G, additional, Li, W, additional, Li, X, additional, Li, X F, additional, Li, Z W, additional, Liang, X H, additional, Liao, J Y, additional, Liu, B S, additional, Liu, H X, additional, Liu, H W, additional, Liu, X J, additional, Lu, X F, additional, Luo, Q, additional, Luo, T, additional, Ma, R C, additional, Ma, X, additional, Meng, B, additional, Nang, Y, additional, Nie, J Y, additional, Ou, G, additional, Ren, X Q, additional, Sai, N, additional, Song, X Y, additional, Sun, L, additional, Tan, Y, additional, Tuo, Y L, additional, Wang, C, additional, Wang, L J, additional, Wang, P J, additional, Wang, W S, additional, Wang, Y S, additional, Wen, X Y, additional, Wu, B Y, additional, Wu, B B, additional, Wu, M, additional, Xiao, G C, additional, Xiao, S, additional, Xiong, S L, additional, Yang, R J, additional, Yang, S, additional, Yang, Yan-Ji, additional, Yang, Yi-Jung, additional, Yi, Q B, additional, Yin, Q Q, additional, You, Y, additional, Zhang, F, additional, Zhang, H M, additional, Zhang, J, additional, Zhang, P, additional, Zhang, W, additional, Zhang, W C, additional, Zhang, Yi, additional, Zhang, Y F, additional, Zhang, Y H, additional, Zhao, H S, additional, Zhao, X F, additional, Zheng, S J, additional, Zheng, Y G, additional, and Zhou, D K, additional

Published
2020
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22. 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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23. Insight-HXMT observations of Swift J0243.6+6124: the evolution of RMS pulse fractions at super-Eddington luminosity

Author

Wang, P J, primary, Kong, L D, additional, Zhang, S, additional, Chen, Y P, additional, Zhang, S N, additional, Qu, J L, additional, Ji, L, additional, Tao, L, additional, Ge, M Y, additional, Lu, F J, additional, Chen, L, additional, Song, L M, additional, Li, T P, additional, Xu, Y P, additional, Cao, X L, additional, Chen, Y, additional, Liu, C Z, additional, Bu, Q C, additional, Cai, C, additional, Chang, Z, additional, Chen, G, additional, Chen, T X, additional, Chen, Y B, additional, Cui, W, additional, Cui, W W, additional, Deng, J K, additional, Dong, Y W, additional, Du, Y Y, additional, Fu, M X, additional, Gao, G H, additional, Gao, H, additional, Gao, M, additional, Gu, Y D, additional, Guan, J, additional, Guo, C C, additional, Han, D W, additional, Huang, Y, additional, Huo, J, additional, Jia, S M, additional, Jiang, L H, additional, Jiang, W C, additional, Jin, J, additional, Jin, Y J, additional, Li, B, additional, Li, C K, additional, Li, G, additional, Li, M S, additional, Li, W, additional, Li, X, additional, Li, X B, additional, Li, X F, additional, Li, Y G, additional, Li, Z W, additional, Liang, X H, additional, Liao, J Y, additional, Liu, B S, additional, Liu, G Q, additional, Liu, H W, additional, Liu, X J, additional, Liu, Y N, additional, Lu, B, additional, Lu, X F, additional, Luo, Q, additional, Luo, T, additional, Ma, X, additional, Meng, B, additional, Nang, Y, additional, Nie, J Y, additional, Ou, G, additional, Sai, N, additional, Shang, R C, additional, Song, X Y, additional, Sun, L, additional, Tan, Y, additional, Tuo, Y L, additional, Wang, C, additional, Wang, G F, additional, Wang, J, additional, Wang, L J, additional, Wang, W S, additional, Wang, Y S, additional, Wen, X Y, additional, Wu, B Y, additional, Wu, B B, additional, Wu, M, additional, Xiao, G C, additional, Xiao, S, additional, Xiong, S L, additional, Yang, J W, additional, Yang, S, additional, Yang, Yan Ji, additional, Yang, Yi Jung, additional, Yi, Q B, additional, Yin, Q Q, additional, You, Y, additional, Zhang, A M, additional, Zhang, C M, additional, Zhang, F, additional, Zhang, H M, additional, Zhang, J, additional, Zhang, T, additional, Zhang, W C, additional, Zhang, W, additional, Zhang, W Z, additional, Zhang, Y, additional, Zhang, Y F, additional, Zhang, Y J, additional, Zhang, Zhao, additional, Zhang, Zhi, additional, Zhang, Z L, additional, Zhao, H S, additional, Zhao, X F, additional, Zheng, S J, additional, Zheng, Y G, additional, Zhou, D K, additional, Zhou, J F, additional, Zhu, Y X, additional, Zhu, Y, additional, and Zhuang, R L, additional

Published
2020
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24. Background model for the Low-Energy Telescope of Insight-HXMT

Author

Liao, Jin-Yuan, primary, Zhang, Shu, additional, Chen, Yong, additional, Zhang, Juan, additional, Jin, Jing, additional, Chang, Zhi, additional, Chen, Yu-Peng, additional, Ge, Ming-Yu, additional, Guo, Cheng-Cheng, additional, Li, Gang, additional, Li, Xiao-Bo, additional, Lu, Fang-Jun, additional, Lu, Xue-Feng, additional, Nie, Jian-Yin, additional, Song, Li-Ming, additional, Yang, Yan-Ji, additional, You, Yuan, additional, Zhao, Hai-Sheng, additional, and Zhang, Shuang-Nan, additional

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

Author

Ji, L, primary, Ducci, L, primary, Santangelo, A, primary, Zhang, S, primary, Suleimanov, V, primary, Tsygankov, S, primary, Doroshenko, V, primary, Nabizadeh, A, primary, Zhang, S N, primary, Ge, M Y, primary, Tao, L, primary, Bu, Q C, primary, Qu, J L, primary, Lu, F J, primary, Chen, L, primary, Song, L M, primary, Li, T P, primary, Xu, Y P, primary, Cao, X L, primary, Chen, Y, primary, Liu, C Z, primary, Cai, C, primary, Chang, Z, primary, Chen, G, primary, Chen, T X, primary, Chen, Y B, primary, Chen, Y P, primary, Cui, W, primary, Cui, W W, primary, Deng, J K, primary, Dong, Y W, primary, Du, Y Y, primary, Fu, M X, primary, Gao, G H, primary, Gao, H, primary, Gao, M, primary, Gu, Y D, primary, Guan, J, primary, Guo, C C, primary, Han, D W, primary, Huang, Y, primary, Huo, J, primary, Jia, S M, primary, Jiang, L H, primary, Jiang, W C, primary, Jin, J, primary, Jin, Y J, primary, Kong, L D, primary, Li, B, primary, Li, C K, primary, Li, G, primary, Li, M S, primary, Li, W, primary, Li, X, primary, Li, X B, primary, Li, X F, primary, Li, Y G, primary, Li, Z W, primary, Liang, X H, primary, Liao, J Y, primary, Liu, B S, primary, Liu, G Q, primary, Liu, H X, primary, Liu, H W, primary, Liu, X J, primary, Liu, Y N, primary, Lu, B, primary, Lu, X F, primary, Luo, Q, primary, Luo, T, primary, Ma, X, primary, Meng, B, primary, Nang, Y, primary, Nie, J Y, primary, Ou, G, primary, Sai, N, primary, Shang, R C, primary, Song, X Y, primary, Sun, L, primary, Tan, Y, primary, Tuo, Y L, primary, Wang, C, primary, Wang, G F, primary, Wang, J, primary, Wang, P J, primary, Wang, W S, primary, Wang, Y S, primary, Wen, X Y, primary, Wu, B Y, primary, Wu, B B, primary, Wu, M, primary, Xiao, G C, primary, Xiao, S, primary, Xiong, S L, primary, Xu, H, primary, Yang, J W, primary, Yang, S, primary, Yang, Yan-Ji, primary, Yang, Yi-Jung, primary, Yi, Q B, primary, Yin, Q Q, primary, You, Y, primary, Zhang, A M, primary, Zhang, C M, primary, Zhang, F, primary, Zhang, H M, primary, Zhang, J, primary, Zhang, P, primary, Zhang, T, primary, Zhang, W, primary, Zhang, W C, primary, Zhang, W Z, primary, Zhang, Yi, primary, Zhang, Y F, primary, Zhang, Y J, primary, Zhang, Y H, primary, Zhang, Yue, primary, Zhang, Zhao, primary, Zhang, Zhi, primary, Zhang, Z L, primary, Zhao, H S, primary, Zhao, X F, primary, Zheng, S J, primary, Zhou, D K, primary, Zhou, J F, primary, Zhu, Y X, primary, Zhu, Y, primary, and Zhuang, R L, primary

Published
2020
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27. 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

28. Numerical Study on Thermal Deformation of Wolter-I Focusing Telescope

Author

王娟 Wang Juan, 文键 Wen Jian, 陈勇 Chen Yong, 杨彦佶 Yang Yan-ji, 张星 Zhang Xing, and 张艺 Zhang Yi

Subjects
Physics, Telescope, Optics, business.industry, law, Thermal deformation, business, Atomic and Molecular Physics, and Optics, law.invention
Published
2020

29. 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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30. 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

31. 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

33. 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

34. 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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35. Measurements of charge transfer efficiency in a proton-irradiated swept charge device

Author

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

Published
2014
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36. Fabrication of Self-Supported Al/Polyimide/Al Film with Thick Supporting Nickel Mesh

Author

Hu, Wei, primary, Chen, Tian Xiang, additional, Sun, Qing Rong, additional, Chen, Yong, additional, Cui, Wei Wei, additional, Zhang, Zi Liang, additional, Li, Wei, additional, Wang, Yu Sa, additional, Han, Da Wei, additional, Wang, Juan, additional, Lu, Bo, additional, Huo, Jia, additional, Li, Mao Shun, additional, Zhang, Yi, additional, Yin, Guo He, additional, Yang, Yan Ji, additional, Liu, Xiao Yan, additional, Zhu, Yue, additional, Li, Cheng Kui, additional, Liu, Yan, additional, and Wu, Di, additional

Published
2013
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37. Low temperature testing and neutron irradiation of a swept charge device on board the HXMT satellite

Author

Wang, Yu-Sa, primary, Chen, Yong, additional, Xu, Yu-Peng, additional, Yang, Yan-Ji, additional, Cui, Wei-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, Li, Zheng-Wei, additional, Li, Wei, additional, Hu, Wei, additional, Zhang, Yi, additional, Lu, Bo, additional, Zhu, Yue, additional, Liu, Yan, additional, Wu, Di, additional, Sun, Qing-Rong, additional, and Zhang, Zi-Liang, additional

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

Author

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

Published
2012
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39. Thermal analysis and expected performance of the low energy instrument on board the HXMT satellite

Author

Wang, Yu-Sa, primary, Chen, Yong, additional, Xu, Yu-Peng, additional, Wang, Juan, additional, Cui, Wei-Wei, additional, Li, Wei, additional, Han, Da-Wei, additional, Zhang, Zi-Liang, additional, Chen, Tian-Xiang, additional, Li, Cheng-Kui, additional, Yang, Yan-Ji, additional, Liu, Xiao-Yan, additional, Huo, Jia, additional, Zhang, Jun-Min, additional, and Zheng, Yi-Qian, additional

Published
2010
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40. [Genetic characterization analysis on the first imported measles virus of genotype D8 in Chinese mainland].

Author

Sun XD, Li CS, Tang X, Li Z, Zhang Y, Tang W, Wang J, Wang HL, Yang YJ, Li J, Yuan ZA, and Xu WB

Subjects
Adolescent, Adult, Aged, Child, Child, Preschool, China, Female, Genotype, Humans, Infant, Male, Measles virus classification, Middle Aged, Molecular Sequence Data, Phylogeny, Travel, Viral Proteins genetics, Young Adult, Measles virology, Measles virus genetics, Measles virus isolation & purification
Abstract

This study analyzed the genetic characterization on first imported measles virus of genotype D8 in Chinese mainland. Serums were collected from the suspicious MV patients to detect IgM antibody in ELISA. Throat swabs were cultured in Vero/SLAM cell line to get measles virus isolates. Part of the nucleotide sequence of the 3' terminus of nucleoprotein (N) gene of these isolates were amplified by RT-PCR, and the amplicons were directly sequenced. The phylogenetic analysis was based on the nucleotide sequence about 456 base pairs of the 3' terminus of nucleoprotein (N) gene. Results showed that it reported 1 105 suspicious measles cases in shanghai, 2012, including 590 confirmed cases and 2 clinical case. The reported morbidity was 2.52 per one hundred thousand. 247 measles viruses were isolated from 984 throat swabs specimen. Most of them belonged to sub-genotype H1a except Shanghai12-239 was genotype D8. The homology of nucleotide and amino acid sequences were 97.8% and 98.6% respectively between Shanghai12-239 and WHO reference strain (Manchester. UNK30.94(D8)AF280803). Those were 89.6%-94.5% and 88.7%-95.3% between Shanghai12-239 and WHO reference strains of other genotypes.

Published
2013

41. [Study on the quality of life among floating population in a community of Shanghai].

Author

Yang YJ, Wang SM, and Wang ZW

Subjects
China, Family Relations, Female, Humans, Male, Quality of Life, Ships, Social Conditions
Abstract

Objective: To discover the current condition of the floating population's quality of life (QOL) in a community of Shanghai and find out the possible influencing factors., Methods: 480 people identified as 'floating', were chosen by systematic sampling method, whose QOL was evaluated by WHOQOL-BREF (Chinese Version). A multiple linear regression model was used to analyze the relationship between the factors and the scores of the four domains., Results: The physical and psychological scores of the floating population were 14.09 +/- 2.09 and 11.28 +/- 2.18 which were lower than the average levels of the Chinese population which were 15.8 +/- 2.9 and 14.3 +/- 2.5. Women showed higher score in the social relationship domain than men (P = 0.017). With the increase of age, the scores of physical and psychological domain were descending (P(Phys.) = 0.030, P(Phych.) = 0.023). The score in every domain was rising when the appetite was better or the family conflicts had a lighter impact on life (P < 0.01)., Conclusion: The QOL of the young females was better than other groups. Considering the whole QOL of the floating population, their physical and psychological demands should be highly concerned.

Published
2007

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