Author: "Wang, J C" / Publication Year Range: Last 3 years - Searchworks@Jio Institute Digital Library Search Results

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102 results on '"Wang, J C"'

1. Detection of two TeV gamma-ray outbursts from NGC 1275 by LHAASO

Author: Cao, Zhen, Aharonian, F., Axikegu, Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, J. T., Cao, Q., Cao, W. Y., Cao, Zhe, Chang, J., Chang, J. F., Chen, A. M., Chen, E. S., Chen, Liang, Chen, Lin, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, M. Y., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, della Volpe, D., Dong, X. Q., Duan, K. K., Fan, J. H., Fan, Y. Z., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, X. T., Feng, Y. L., Gabici, S., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Giacinti, G., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. Y., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, B. W., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S. C., Huang, D. H., Huang, T. Q., Huang, W. J., Huang, X. T., Huang, X. Y., Huang, Y., Huang, Z. C., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, X. W., Jiang, Z. J., Jin, M., Kang, M. M., Ke, T., Kuleshov, D., Kurinov, K., Li, B. B., Li, Cheng, Li, Cong, Li, D., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, Jian, Li, Jie, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Lu, R., Luo, Q., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Min, Z., Mitthumsiri, W., Mu, H. J., Nan, Y. C., Neronov, A., Ou, Z. W., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Sáiz, A., Semikoz, D., Shao, C. Y., Shao, L., Shchegolev, O., Sheng, X. D., Shu, F. W., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Q. W., Tang, Z. B., Tian, W. W., Wang, C., Wang, C. B., Wang, G. W., Wang, H. G., Wang, H. H., Wang, J. C., Wang, K., Wang, L. P., Wang, L. Y., Wang, P. H., Wang, R., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, X. F., Wu, Y. S., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, G. G., Xin, Y. L., Xing, Y., Xiong, Z., Xu, D. L., Xu, R. F., Xu, R. X., Xu, W. L., Xue, L., Yan, D. H., Yan, J. Z., Yan, T., Yang, C. W., Yang, F., Yang, F. F., Yang, H. W., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zha, M., Zhang, B. B., Zhang, F., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, L. X., Zhang, Li, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zhou, B., Zhou, H., Zhou, J. N., Zhou, M., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo., X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Water Cherenkov Detector Array (WCDA) is one of the components of Large High Altitude Air Shower Observatory (LHAASO) and can monitor any sources over two-thirds of the sky for up to 7 hours per day with >98\% duty cycle. In this work, we report the detection of two outbursts of the Fanaroff-Riley I radio galaxy NGC 1275 that were detected by LHAASO-WCDA between November 2022 and January 2023 with statistical significance of 5.2~$\sigma$ and 8.3~$\sigma$. The observed spectral energy distribution in the range from 500 GeV to 3 TeV is fitted by a power-law with a best-fit spectral index of $\alpha=-3.37\pm0.52$ and $-3.35\pm0.29$, respectively. The outburst flux above 0.5~TeV was ($4.55\pm 4.21)\times~10^{-11}~\rm cm^{-2}~s^{-1}$ and ($3.45\pm 1.78)\times~10^{-11}~\rm cm^{-2}~s^{-1}$, corresponding to 60\%, 45\% of Crab Nebula flux. Variation analysis reveals the variability time-scale of days at the TeV energy band. A simple test by one-zone synchrotron self-Compton model reproduces the data in the gamma-ray band well., Comment: 11 pages, 8 figures, 3 tables
Published: 2024

2. LHAASO detection of very-high-energy gamma-ray emission surrounding PSR J0248+6021

Author: Cao, Zhen, Aharonian, F., An, Q., Axikegu, Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, J. T., Cao, Q., Cao, W. Y., Cao, Zhe, Chang, J., Chang, J. F., Chen, A. M., Chen, E. S., Chen, Liang, Chen, Lin, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, M. Y., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, Dong, X. Q., Duan, K. K., Fan, J. H., Fan, Y. Z., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, X. T., Feng, Y. L., Gabici, S., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Giacinti, G., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. Y., He, X. B., He, Y., Hor, Y. K., Hou, B. W., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S. C., Huang, D. H., Huang, T. Q., Huang, W. J., Huang, X. T., Huang, X. Y., Huang, Y., Huang, Z. C., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, X. W., Jiang, Z. J., Jin, M., Kang, M. M., Ke, T., Kuleshov, D., Kurinov, K., Li, B. B., Li, Cheng, Li, Cong, Li, D., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, Jian, Li, Jie, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Lu, R., Luo, Q., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Min, Z., Mitthumsiri, W., Mu, H. J., Nan, Y. C., Neronov, A., Ou, Z. W., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Sáiz, A., Semikoz, D., Shao, C. Y., Shao, L., Shchegolev, O., Sheng, X. D., Shu, F. W., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Q. W., Tang, Z. B., Tian, W. W., Wang, C., Wang, C. B., Wang, G. W., Wang, H. G., Wang, H. H., Wang, J. C., Wang, K., Wang, L. P., Wang, L. Y., Wang, P. H., Wang, R., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, X. F., Wu, Y. S., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, G. G., Xin, Y. L., Xing, Y., Xiong, Z., Xu, D. L., Xu, R. F., Xu, R. X., Xu, W. L., Xue, L., Yan, D. H., Yan, J. Z., Yan, T., Yang, C. W., Yang, F., Yang, F. F., Yang, H. W., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zha, M., Zhang, B. B., Zhang, F., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, L. X., Zhang, Li, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zheng, J. H., Zhou, B., Zhou, H., Zhou, J. N., Zhou, M., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., Zou, Y. C., and Zuo, X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the detection of an extended very-high-energy (VHE) gamma-ray source coincident with the locations of middle-aged (62.4~\rm kyr) pulsar PSR J0248+6021, by using the LHAASO-WCDA data of live 796 days and LHAASO-KM2A data of live 1216 days. A significant excess of \gray induced showers is observed both by WCDA in energy bands of 1-25~\rm TeV and KM2A in energy bands of $>$ 25~\rm TeV with 7.3 $\sigma$ and 13.5 $\sigma$, respectively. The best-fit position derived through WCDA data is R.A. = 42.06$^\circ \pm$ 0.12$^\circ$ and Dec. = 60.24$^\circ \pm $ 0.13$^\circ$ with an extension of 0.69$^\circ\pm$0.15$^\circ$ and that of the KM2A data is R.A.= 42.29$^\circ \pm $ 0.13$^\circ$ and Dec. = 60.38$^\circ \pm$ 0.07$^\circ$ with an extension of 0.37$^\circ\pm$0.07$^\circ$. No clear extended multiwavelength counterpart of this LHAASO source has been found from the radio band to the GeV band. The most plausible explanation of the VHE \gray emission is the inverse Compton process of highly relativistic electrons and positrons injected by the pulsar. These electrons/positrons are hypothesized to be either confined within the pulsar wind nebula or to have already escaped into the interstellar medium, forming a pulsar halo., Comment: 12 pages, 10 figures, Accepted by Sci. China-Phys. Mech. Astron
Published: 2024

3. Constraints on Ultra Heavy Dark Matter Properties from Dwarf Spheroidal Galaxies with LHAASO Observations

Author: Cao, Zhen, Aharonian, F., An, Q., Axikegu, Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, J. T., Cao, Q., Cao, W. Y., Cao, Zhe, Chang, J., Chang, J. F., Chen, A. M., Chen, E. S., Chen, Liang, Chen, Lin, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, M. Y., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, della Volpe, D., Dong, X. Q., Duan, K. K., Fan, J. H., Fan, Y. Z., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, X. T., Feng, Y. L., Gabici, S., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Giacinti, G., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. Y., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, B. W., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S. C., Huang, D. H., Huang, T. Q., Huang, W. J., Huang, X. T., Huang, X. Y., Huang, Y., Huang, Z. C., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, X. W., Jiang, Z. J., Jin, M., Kang, M. M., Ke, T., Kuleshov, D., Kurinov, K., Li, B. B., Li, Cheng, Li, Cong, Li, D., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, Jian, Li, Jie, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Lu, R., Luo, Q., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Min, Z., Mitthumsiri, W., Mu, H. J., Nan, Y. C., Neronov, A., Ou, Z. W., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Saiz, A., Semikoz, D., Shao, C. Y., Shao, L., Shchegolev, O., Sheng, X. D., Shu, F. W., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Q. W., Tang, Z. B., Tian, W. W., Wang, C., Wang, C. B., Wang, G. W., Wang, H. G., Wang, H. H., Wang, J. C., Wang, K., Wang, L. P., Wang, L. Y., Wang, P. H., Wang, R., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, X. F., Wu, Y. S., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, G. G., Xin, Y. L., Xing, Y., Xiong, Z., Xu, D. L., Xu, R. F., Xu, R. X., Xu, W. L., Xue, L., Yan, D. H., Yan, J. Z., Yan, T., Yang, C. W., Yang, F., Yang, F. F., Yang, H. W., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zha, M., Zhang, B. B., Zhang, F., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, L. X., Zhang, Li, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zhou, B., Zhou, H., Zhou, J. N., Zhou, M., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo, X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
Abstract: In this work we try to search for signals generated by ultra-heavy dark matter at the Large High Altitude Air Shower Observatory (LHAASO) data. We look for possible gamma-ray by dark matter annihilation or decay from 16 dwarf spheroidal galaxies in the field of view of LHAASO. Dwarf spheroidal galaxies are among the most promising targets for indirect detection of dark matter which have low fluxes of astrophysical $\gamma$-ray background while large amount of dark matter. By analyzing more than 700 days observational data at LHAASO, no significant dark matter signal from 1 TeV to 1 EeV is detected. Accordingly we derive the most stringent constraints on the ultra-heavy dark matter annihilation cross-section up to EeV. The constraints on the lifetime of dark matter in decay mode are also derived., Comment: 17 pages, 12 figures, accepted by PRL
Published: 2024

4. Data quality control system and long-term performance monitor of the LHAASO-KM2A

Author: Cao, Zhen, Aharonian, F., Axikegu, Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Bian, W., Bukevich, A. V., Cao, Q., Cao, W. Y., Cao, Zhe, Chang, J., Chang, J. F., Chen, A. M., Chen, E. S., Chen, H. X., Chen, Liang, Chen, Lin, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, M. Y., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, Dong, X. Q., Duan, K. K., Fan, J. H., Fan, Y. Z., Fang, J., Fang, J. H., Fang, K., Feng, C. F., Feng, H., Feng, L., Feng, S. H., Feng, X. T., Feng, Y., Feng, Y. L., Gabici, S., Gao, B., Gao, C. D., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Giacinti, G., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., Hasan, M., He, H. H., He, H. N., He, J. Y., He, Y., Hor, Y. K., Hou, B. W., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S. C., Huang, D. H., Huang, T. Q., Huang, W. J., Huang, X. T., Huang, X. Y., Huang, Y., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, X. W., Jiang, Z. J., Jin, M., Kang, M. M., Karpikov, I., Kuleshov, D., Kurinov, K., Li, B. B., Li, C. M., Li, Cheng, Li, Cong, Li, D., Li, F., Li, H. B., Li, H. C., Li, Jian, Li, Jie, Li, K., Li, S. D., Li, W. L., Li, X. R., Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, D. B., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Luo, Q., Luo, Y., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Min, Z., Mitthumsiri, W., Mu, H. J., Nan, Y. C., Neronov, A., Ou, L. J., Pattarakijwanich, P., Pei, Z. Y., Qi, J. C., Qi, M. Y., Qiao, B. Q., Qin, J. J., Raza, A., Ruffolo, D., Sáiz, A., Saeed, M., Semikoz, D., Shao, L., Shchegolev, O., Sheng, X. D., Shu, F. W., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, D. X., Sun, Q. N., Sun, X. N., Sun, Z. B., Takata, J., Tam, P. H. T., Tang, Q. W., Tang, R., Tang, Z. B., Tian, W. W., Wang, C., Wang, C. B., Wang, G. W., Wang, H. G., Wang, H. H., Wang, J. C., Wang, Kai, Wang, L. P., Wang, L. Y., Wang, P. H., Wang, R., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, Q. W., Wu, S., Wu, X. F., Wu, Y. S., Xi, S. Q., Xia, J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, Y. L., Xing, Y., Xiong, D. R., Xiong, Z., Xu, D. L., Xu, R. F., Xu, R. X., Xu, W. L., Xue, L., Yan, D. H., Yan, J. Z., Yan, T., Yang, C. W., Yang, C. Y., Yang, F., Yang, F. F., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, W. X., Yao, Y. H., Yao, Z. G., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zha, M., Zhang, B. B., Zhang, F., Zhang, H., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, Li, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zhao, X. H., Zheng, F., Zhong, W. J., Zhou, B., Zhou, H., Zhou, J. N., Zhou, M., Zhou, P., Zhou, R., Zhou, X. X., Zhu, B. Y., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., Zou, Y. C., and Zuo, X.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract: The KM2A is the largest sub-array of the Large High Altitude Air Shower Observatory (LHAASO). It consists of 5216 electromagnetic particle detectors (EDs) and 1188 muon detectors (MDs). The data recorded by the EDs and MDs are used to reconstruct primary information of cosmic ray and gamma-ray showers. This information is used for physical analysis in gamma-ray astronomy and cosmic ray physics. To ensure the reliability of the LHAASO-KM2A data, a three-level quality control system has been established. It is used to monitor the status of detector units, stability of reconstructed parameters and the performance of the array based on observations of the Crab Nebula and Moon shadow. This paper will introduce the control system and its application on the LHAASO-KM2A data collected from August 2021 to July 2023. During this period, the pointing and angular resolution of the array were stable. From the observations of the Moon shadow and Crab Nebula, the results achieved using the two methods are consistent with each other. According to the observation of the Crab Nebula at energies from 25 TeV to 100 TeV, the time averaged pointing errors are estimated to be $-0.003^{\circ} \pm 0.005^{\circ}$ and $0.001^{\circ} \pm 0.006^{\circ}$ in the R.A. and Dec directions, respectively., Comment: 15 pages, 9 figures
Published: 2024

5. Discovery of Very-high-energy Gamma-ray Emissions from the Low Luminosity AGN NGC 4278 by LHAASO

Author: Cao, Zhen, Aharonian, F., An, Q., Axikegu, Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, J. T., Cao, Q., Cao, W. Y., Cao, Zhe, Chang, J., Chang, J. F., Chen, A. M., Chen, E. S., Chen, Liang, Chen, Lin, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, M. Y., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, Dong, X. Q., Duan, K. K., Fan, J. H., Fan, Y. Z., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, X. T., Feng, Y. L., Gabici, S., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Giacinti, G., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. Y., He, X. B., He, Y., Hor, Y. K., Hou, B. W., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S. C., Huang, D. H., Huang, T. Q., Huang, W. J., Huang, X. T., Huang, X. Y., Huang, Y., Huang, Z. C., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, X. W., Jiang, Z. J., Jin, M., Kang, M. M., Ke, T., Kuleshov, D., Kurinov, K., Li, B. B., Li, Cheng, Li, Cong, Li, D., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, Jian, Li, Jie, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Lu, R., Luo, Q., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Min, Z., Mitthumsiri, W., Mu, H. J., Nan, Y. C., Neronov, A., Ou, Z. W., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Sáiz, A., Semikoz, D., Shao, C. Y., Shao, L., Shchegolev, O., Sheng, X. D., Shu, F. W., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Q. W., Tang, Z. B., Tian, W. W., Wang, C., Wang, C. B., Wang, G. W., Wang, H. G., Wang, H. H., Wang, J. C., Wang, K., Wang, L. P., Wang, L. Y., Wang, P. H., Wang, R., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, X. F., Wu, Y. S., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, G. G., Xin, Y. L., Xing, Y., Xiong, Z., Xu, D. L., Xu, R. F., Xu, R. X., Xu, W. L., Xue, L., Yan, D. H., Yan, J. Z., Yan, T., Yang, C. W., Yang, F., Yang, F. F., Yang, H. W., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zha, M., Zhang, B. B., Zhang, F., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, L. X., Zhang, Li, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zheng, J. H., Zhou, B., Zhou, H., Zhou, J. N., Zhou, M., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., Zou, Y. C., and Zuo, X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The first source catalog of Large High Altitude Air Shower Observatory reported the detection of a very-high-energy gamma ray source, 1LHAASO J1219+2915. In this paper a further detailed study of the spectral and temporal behavior of this point-like source have been carried. The best-fit position of the TeV source ($\rm{RA}=185.05^{\circ}\pm0.04^{\circ}$, $\rm{Dec}=29.25^{\circ}\pm0.03^{\circ}$) is compatible with NGC 4278 within $\sim0.03$ degree. Variation analysis shows an indication of the variability at a few months level in the TeV band, which is consistent with low frequency observations. Based on these observations, we report the detection of TeV $\gamma$-ray emissions from this low-luminosity AGN NGC 4278. The observations by LHAASO-WCDA during active period has a significance level of 8.8\,$\sigma$ with best-fit photon spectral index $\varGamma=2.56\pm0.14$ and a flux $f_{1-10\,\rm{TeV}}=(7.0\pm1.1_{\rm{sta}}\pm0.35_{\rm{syst}})\times10^{-13}\,\rm{photons\,cm^{-2}\,s^{-1}}$, or approximately $5\%$ of the Crab Nebula. The discovery of VHE from NGC 4278 indicates that the compact, weak radio jet can efficiently accelerate particles and emit TeV photons., Comment: 11 pages, 5 figures
Published: 2024

6. LHAASO-KM2A detector simulation using Geant4

Author: Cao, Zhen, Aharonian, F., An, Q., Axikegu, Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, J. T., Cao, Q., Cao, W. Y., Cao, Zhe, Chang, J., Chang, J. F., Chen, A. M., Chen, E. S., Chen, Liang, Chen, Lin, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, M. Y., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, Dong, X. Q., Duan, K. K., Fan, J. H., Fan, Y. Z., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, X. T., Feng, Y. L., Gabici, S., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Giacinti, G., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. Y., He, X. B., He, Y., Hor, Y. K., Hou, B. W., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S. C., Huang, D. H., Huang, T. Q., Huang, W. J., Huang, X. T., Huang, X. Y., Huang, Y., Huang, Z. C., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, X. W., Jiang, Z. J., Jin, M., Kang, M. M., Ke, T., Kuleshov, D., Kurinov, K., Li, B. B., Li, Cheng, Li, Cong, Li, D., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, Jian, Li, Jie, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Lu, R., Luo, Q., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Min, Z., Mitthumsiri, W., Mu, H. J., Nan, Y. C., Neronov, A., Ou, Z. W., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Sáiz, A., Semikoz, D., Shao, C. Y., Shao, L., Shchegolev, O., Sheng, X. D., Shu, F. W., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Q. W., Tang, Z. B., Tian, W. W., Wang, C., Wang, C. B., Wang, G. W., Wang, H. G., Wang, H. H., Wang, J. C., Wang, K., Wang, L. P., Wang, L. Y., Wang, P. H., Wang, R., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, X. F., Wu, Y. S., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, G. G., Xin, Y. L., Xing, Y., Xiong, Z., Xu, D. L., Xu, R. F., Xu, R. X., Xu, W. L., Xue, L., Yan, D. H., Yan, J. Z., Yan, T., Yang, C. W., Yang, F., Yang, F. F., Yang, H. W., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zha, M., Zhang, B. B., Zhang, F., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, L. X., Zhang, Li, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zheng, J. H., Zhou, B., Zhou, H., Zhou, J. N., Zhou, M., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo, X.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: KM2A is one of the main sub-arrays of LHAASO, working on gamma ray astronomy and cosmic ray physics at energies above 10 TeV. Detector simulation is the important foundation for estimating detector performance and data analysis. It is a big challenge to simulate the KM2A detector in the framework of Geant4 due to the need to track numerous photons from a large number of detector units (>6000) with large altitude difference (30 m) and huge coverage (1.3 km^2). In this paper, the design of the KM2A simulation code G4KM2A based on Geant4 is introduced. The process of G4KM2A is optimized mainly in memory consumption to avoid memory overffow. Some simpliffcations are used to signiffcantly speed up the execution of G4KM2A. The running time is reduced by at least 30 times compared to full detector simulation. The particle distributions and the core/angle resolution comparison between simulation and experimental data of the full KM2A array are also presented, which show good agreement.
Published: 2024
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7. Measurements of All-Particle Energy Spectrum and Mean Logarithmic Mass of Cosmic Rays from 0.3 to 30 PeV with LHAASO-KM2A

Author: The LHAASO Collaboration, Cao, Zhen, Aharonian, F., An, Q., Axikegu, A., Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, J. T., Cao, Q., Cao, W. Y., Cao, Zhe, Chang, J., Chang, J. F., Chen, A. M., Chen, E. S., Chen, Liang, Chen, Lin, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, M. Y., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, della Volpe, D., Dong, X. Q., Duan, K. K., Fan, J. H., Fan, Y. Z., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, X. T., Feng, Y. L., Gabici, S., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Giacinti, G., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. Y., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, B. W., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S. C., Huang, D. H., Huang, T. Q., Huang, W. J., Huang, X. T., Huang, X. Y., Huang, Y., Huang, Z. C., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, X. W., Jiang, Z. J., Jin, M., Kang, M. M., Ke, T., Kuleshov, D., Kurinov, K., Li, B. B., Li, Cheng, Li, Cong, Li, D., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, Jian, Li, Jie, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Lu, R., Luo, Q., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Min, Z., Mitthumsiri, W., Mu, H. J., Nan, Y. C., Neronov, A., Ou, Z. W., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Sáiz, A., Semikoz, D., Shao, C. Y., Shao, L., Shchegolev, O., Sheng, X. D., Shu, F. W., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Q. W., Tang, Z. B., Tian, W. W., Wang, C., Wang, C. B., Wang, G. W., Wang, H. G., Wang, H. H., Wang, J. C., Wang, K., Wang, L. P., Wang, L. Y., Wang, P. H., Wang, R., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, X. F., Wu, Y. S., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, G. G., Xin, Y. L., Xing, Y., Xiong, Z., Xu, D. L., Xu, R. F., Xu, R. X., Xu, W. L., Xue, L., Yan, D. H., Yan, J. Z., Yan, T., Yang, C. W., Yang, F., Yang, F. F., Yang, H. W., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zha, M., Zhang, B. B., Zhang, F., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, L. X., Zhang, Li, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zhou, B., Zhou, H., Zhou, J. N., Zhou, M., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo, X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the measurements of all-particle energy spectrum and mean logarithmic mass of cosmic rays in the energy range of 0.3-30 PeV using data collected from LHAASO-KM2A between September 2021 and December 2022, which is based on a nearly composition-independent energy reconstruction method, achieving unprecedented accuracy. Our analysis reveals the position of the knee at $3.67 \pm 0.05 \pm 0.15$ PeV. Below the knee, the spectral index is found to be -$2.7413 \pm 0.0004 \pm 0.0050$, while above the knee, it is -$3.128 \pm 0.005 \pm 0.027$, with the sharpness of the transition measured with a statistical error of 2%. The mean logarithmic mass of cosmic rays is almost heavier than helium in the whole measured energy range. It decreases from 1.7 at 0.3 PeV to 1.3 at 3 PeV, representing a 24% decline following a power law with an index of -$0.1200 \pm 0.0003 \pm 0.0341$. This is equivalent to an increase in abundance of light components. Above the knee, the mean logarithmic mass exhibits a power law trend towards heavier components, which is reversal to the behavior observed in the all-particle energy spectrum. Additionally, the knee position and the change in power-law index are approximately the same. These findings suggest that the knee observed in the all-particle spectrum corresponds to the knee of the light component, rather than the medium-heavy components., Comment: 8 pages, 3 figures
Published: 2024
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8. Does or did the supernova remnant Cassiopeia A operate as a PeVatron?

Author: Cao, Zhen, Aharonian, F., An, Q., Axikegu, Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, J. T., Cao, Q., Cao, W. Y., Cao, Zhe, Chang, J., Chang, J. F., Chen, A. M., Chen, E. S., Chen, Liang, Chen, Lin, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, M. Y., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, della Volpe, D., Dong, X. Q., Duan, K. K., Fan, J. H., Fan, Y. Z., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, X. T., Feng, Y. L., Gabici, S., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Giacinti, G., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. Y., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, B. W., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S. C., Huang, D. H., Huang, T. Q., Huang, W. J., Huang, X. T., Huang, X. Y., Huang, Y., Huang, Z. C., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, X. W., Jiang, Z. J., Jin, M., Kang, M. M., Ke, T., Kuleshov, D., Kurinov, K., Li, B. B., Li, Cheng, Li, Cong, Li, D., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, Jian, Li, Jie, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Lu, R., Luo, Q., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Min, Z., Mitthumsiri, W., Mu, H. J., Nan, Y. C., Neronov, A., Ou, Z. W., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Sáiz, A., Semikoz, D., Shao, C. Y., Shao, L., Shchegolev, O., Sheng, X. D., Shu, F. W., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Q. W., Tang, Z. B., Tian, W. W., Wang, C., Wang, C. B., Wang, G. W., Wang, H. G., Wang, H. H., Wang, J. C., Wang, K., Wang, L. P., Wang, L. Y., Wang, P. H., Wang, R., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, X. F., Wu, Y. S., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, G. G., Xin, Y. L., Xing, Y., Xiong, Z., Xu, D. L., Xu, R. F., Xu, R. X., Xu, W. L., Xue, L., Yan, D. H., Yan, J. Z., Yan, T., Yang, C. W., Yang, F., Yang, F. F., Yang, H. W., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zha, M., Zhang, B. B., Zhang, F., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, L. X., Zhang, Li, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zhou, B., Zhou, H., Zhou, J. N., Zhou, M., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo., X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: For decades, supernova remnants (SNRs) have been considered the prime sources of Galactic Cosmic rays (CRs). But whether SNRs can accelerate CR protons to PeV energies and thus dominate CR flux up to the knee is currently under intensive theoretical and phenomenological debate. The direct test of the ability of SNRs to operate as CR PeVatrons can be provided by ultrahigh-energy (UHE; $E_\gamma \geq 100$~TeV) $\gamma$-rays. In this context, the historical SNR Cassiopeia A (Cas A) is considered one of the most promising target for UHE observations. This paper presents the observation of Cas A and its vicinity by the LHAASO KM2A detector. The exceptional sensitivity of LHAASO KM2A in the UHE band, combined with the young age of Cas A, enabled us to derive stringent model-independent limits on the energy budget of UHE protons and nuclei accelerated by Cas A at any epoch after the explosion. The results challenge the prevailing paradigm that Cas A-type SNRs are major suppliers of PeV CRs in the Milky Way., Comment: 11 pages, 3 figures, Accepted by the APJL
Published: 2023

9. Very high energy gamma-ray emission beyond 10 TeV from GRB 221009A

Author: Cao, Zhen, Aharonian, F., An, Q., Axikegu, A., Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, J. T., Cao, Q., Cao, W. Y., Cao, Zhe, Chang, J., Chang, J. F., Chen, A. M., Chen, E. S., Chen, Liang, Chen, Lin, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, M. Y., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, della Volpe, D., Dong, X. Q., Duan, K. K., Fan, J. H., Fan, Y. Z., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, X. T., Feng, Y. L., Gabici, S., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Giacinti, G., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. Y., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, B. W., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S. C., Huang, D. H., Huang, T. Q., Huang, W. J., Huang, X. T., Huang, X. Y., Huang, Y., Huang, Z. C., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, X. W., Jiang, Z. J., Jin, M., Kang, M. M., Ke, T., Kuleshov, D., Kurinov, K., Li, B. B., Li, Cheng, Li, Cong, Li, D., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, Jian, Li, Jie, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Lu, R., Luo, Q., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Min, Z., Mitthumsiri, W., Mu, H. J., Nan, Y. C., Neronov, A., Ou, Z. W., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Sáiz, A., Semikoz, D., Shao, C. Y., Shao, L., Shchegolev, O., Sheng, X. D., Shu, F. W., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Q. W., Tang, Z. B., Tian, W. W., Wang, C., Wang, C. B., Wang, G. W., Wang, H. G., Wang, H. H., Wang, J. C., Wang, K., Wang, L. P., Wang, L. Y., Wang, P. H., Wang, R., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, X. F., Wu, Y. S., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, G. G., Xin, Y. L., Xing, Y., Xiong, Z., Xu, D. L., Xu, R. F., Xu, R. X., Xu, W. L., Xue, L., Yan, D. H., Yan, J. Z., Yan, T., Yang, C. W., Yang, F., Yang, F. F., Yang, H. W., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zha, M., Zhang, B. B., Zhang, F., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, L. X., Zhang, Li, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zhou, B., Zhou, H., Zhou, J. N., Zhou, M., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo, X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The highest energy gamma-rays from gamma-ray bursts (GRBs) have important implications for their radiation mechanism. Here we report for the first time the detection of gamma-rays up to 13 TeV from the brightest GRB 221009A by the Large High Altitude Air-shower Observatory (LHAASO). The LHAASO-KM2A detector registered more than 140 gamma-rays with energies above 3 TeV during 230$-$900s after the trigger. The intrinsic energy spectrum of gamma-rays can be described by a power-law after correcting for extragalactic background light (EBL) absorption. Such a hard spectrum challenges the synchrotron self-Compton (SSC) scenario of relativistic electrons for the afterglow emission above several TeV. Observations of gamma-rays up to 13 TeV from a source with a measured redshift of z=0.151 hints more transparency in intergalactic space than previously expected. Alternatively, one may invoke new physics such as Lorentz Invariance Violation (LIV) or an axion origin of very high energy (VHE) signals., Comment: 49pages, 11figures
Published: 2023
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10. Research on the Dynamic and Reliability of Planar Multi-Link Mechanisms with Multiple Clearances

Author: Lin, Y. P., Wang, J. C., Zhang, J. L., An, M. X., and Jiang, S.
Published: 2024
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11. The First LHAASO Catalog of Gamma-Ray Sources

Author: Cao, Zhen, Aharonian, F., An, Q., Axikegu, Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, J. T., Cao, Q., Cao, W. Y., Cao, Zhe, Chang, J., Chang, J. F., Chen, A. M., Chen, E. S., Chen, Liang, Chen, Lin, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, M. Y., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, della Volpe, D., Dong, X. Q., Duan, K. K., Fan, J. H., Fan, Y. Z., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, X. T., Feng, Y. L., Gabici, S., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Giacinti, G., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. Y., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, B. W., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S. C., Huang, D. H., Huang, T. Q., Huang, W. J., Huang, X. T., Huang, X. Y., Huang, Y., Huang, Z. C., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, X. W., Jiang, Z. J., Jin, M., Kang, M. M., Ke, T., Kuleshov, D., Kurinov, K., Li, B. B., Li, Cheng, Li, Cong, Li, D., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, Jian, Li, Jie, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Lu, R., Luo, Q., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Min, Z., Mitthumsiri, W., Mu, H. J., Nan, Y. C., Neronov, A., Ou, Z. W., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Sáiz, A., Semikoz, D., Shao, C. Y., Shao, L., Shchegolev, O., Sheng, X. D., Shu, F. W., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Q. W., Tang, Z. B., Tian, W. W., Wang, C., Wang, C. B., Wang, G. W., Wang, H. G., Wang, H. H., Wang, J. C., Wang, K., Wang, L. P., Wang, L. Y., Wang, P. H., Wang, R., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, X. F., Wu, Y. S., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, G. G., Xin, Y. L., Xing, Y., Xiong, Z., Xu, D. L., Xu, R. F., Xu, R. X., Xu, W. L., Xue, L., Yan, D. H., Yan, J. Z., Yan, T., Yang, C. W., Yang, F., Yang, F. F., Yang, H. W., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zha, M., Zhang, B. B., Zhang, F., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, L. X., Zhang, Li, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zhou, B., Zhou, H., Zhou, J. N., Zhou, M., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo., X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
Abstract: We present the first catalog of very-high energy and ultra-high energy gamma-ray sources detected by the Large High Altitude Air Shower Observatory (LHAASO). The catalog was compiled using 508 days of data collected by the Water Cherenkov Detector Array (WCDA) from March 2021 to September 2022 and 933 days of data recorded by the Kilometer Squared Array (KM2A) from January 2020 to September 2022. This catalog represents the main result from the most sensitive large coverage gamma-ray survey of the sky above 1 TeV, covering declination from $-$20$^{\circ}$ to 80$^{\circ}$. In total, the catalog contains 90 sources with an extended size smaller than $2^\circ$ and a significance of detection at $> 5\sigma$. Based on our source association criteria, 32 new TeV sources are proposed in this study. Among the 90 sources, 43 sources are detected with ultra-high energy ($E > 100$ TeV) emission at $> 4\sigma$ significance level. We provide the position, extension, and spectral characteristics of all the sources in this catalog., Comment: 40 pages, 13 figures, 4 tables
Published: 2023
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12. Measurement of ultra-high-energy diffuse gamma-ray emission of the Galactic plane from 10 TeV to 1 PeV with LHAASO-KM2A

Author: Cao, Zhen, Aharonian, F., An, Q., Axikegu, Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, J. T., Cao, Q., Cao, W. Y., Cao, Zhe, Chang, J., Chang, J. F., Chen, A. M., Chen, E. S., Chen, Liang, Chen, Lin, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, M. Y., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, della Volpe, D., Dong, X. Q., Duan, K. K., Fan, J. H., Fan, Y. Z., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, X. T., Feng, Y. L., Gabici, S., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Giacinti, G., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. Y., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, B. W., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S. C., Huang, D. H., Huang, T. Q., Huang, W. J., Huang, X. T., Huang, X. Y., Huang, Y., Huang, Z. C., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, X. W., Jiang, Z. J., Jin, M., Kang, M. M., Ke, T., Kuleshov, D., Kurinov, K., Li, B. B., Li, Cheng, Li, Cong, Li, D., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, Jian, Li, Jie, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Lu, R., Luo, Q., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Min, Z., Mitthumsiri, W., Mu, H. J., Nan, Y. C., Neronov, A., Ou, Z. W., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Saiz, A., Semikoz, D., Shao, C. Y., Shao, L., Shchegolev, O., Sheng, X. D., Shu, F. W., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Q. W., Tang, Z. B., Tian, W. W., Wang, C., Wang, C. B., Wang, G. W., Wang, H. G., Wang, H. H., Wang, J. C., Wang, K., Wang, L. P., Wang, L. Y., Wang, P. H., Wang, R., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, X. F., Wu, Y. S., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, G. G., Xin, Y. L., Xing, Y., Xiong, Z., Xu, D. L., Xu, R. F., Xu, R. X., Xu, W. L., Xue, L., Yan, D. H., Yan, J. Z., Yan, T., Yang, C. W., Yang, F., Yang, F. F., Yang, H. W., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zha, M., Zhang, B. B., Zhang, F., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, L. X., Zhang, Li, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zhou, B., Zhou, H., Zhou, J. N., Zhou, M., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo, X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The diffuse Galactic $\gamma$-ray emission, mainly produced via interactions between cosmic rays and the interstellar medium and/or radiation field, is a very important probe of the distribution, propagation, and interaction of cosmic rays in the Milky Way. In this work we report the measurements of diffuse $\gamma$-rays from the Galactic plane between 10 TeV and 1 PeV energies, with the square kilometer array of the Large High Altitude Air Shower Observatory (LHAASO). Diffuse emissions from the inner ($15^{\circ}10$~TeV). The energy spectrum in the inner Galaxy regions can be described by a power-law function with an index of $-2.99\pm0.04$, which is different from the curved spectrum as expected from hadronic interactions between locally measured cosmic rays and the line-of-sight integrated gas content. Furthermore, the measured flux is higher by a factor of $\sim3$ than the prediction. A similar spectrum with an index of $-2.99\pm0.07$ is found in the outer Galaxy region, and the absolute flux for $10\lesssim E\lesssim60$ TeV is again higher than the prediction for hadronic cosmic ray interactions. The latitude distributions of the diffuse emission are consistent with the gas distribution, while the longitude distributions show clear deviation from the gas distribution. The LHAASO measurements imply that either additional emission sources exist or cosmic ray intensities have spatial variations., Comment: 12 pages, 8 figures, 5 tables; accepted for publication in Physical Review Letters; source mask file provided as ancillary file
Published: 2023
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13. Correction: The HDAC inhibitor, MPT0E028, enhances erlotinib induced cell death in EGFR-TKI-resistant NSCLC cells

Author: Chen, M. -C, Chen, C. -H, Wang, J. -C, Tsai, A. -C, Liou, J. -P, Pan, S. -L, and Teng, C. -M
Published: 2024
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14. STCF Conceptual Design Report: Volume 1 -- Physics & Detector

Author: Achasov, M., Ai, X. C., Aliberti, R., An, L. P., An, Q., Bai, X. Z., Bai, Y., Bakina, O., Barnyakov, A., Blinov, V., Bobrovnikov, V., Bodrov, D., Bogomyagkov, A., Bondar, A., Boyko, I., Bu, Z. H., Cai, F. M., Cai, H., Cao, J. J., Cao, Q. H., Cao, Z., Chang, Q., Chao, K. T., Chen, D. Y., Chen, H., Chen, H. X., Chen, J. F., Chen, K., Chen, L. L., Chen, P., Chen, S. L., Chen, S. M., Chen, S., Chen, S. P., Chen, W., Chen, X. F., Chen, X., Chen, Y., Chen, Y. Q., Cheng, H. Y., Cheng, J., Cheng, S., Dai, J. P., Dai, L. Y., Dai, X. C., Dedovich, D., Denig, A., Denisenko, I., Ding, D. Z., Dong, L. Y., Dong, W. H., Druzhinin, V., Du, D. S., Du, Y. J., Du, Z. G., Duan, L. M., Epifanov, D., Fan, Y. L., Fang, S. S., Fang, Z. J., Fedotovich, G., Feng, C. Q., Feng, X., Feng, Y. T., Fu, J. L., Gao, J., Ge, P. S., Geng, C. Q., Geng, L. S., Gilman, A., Gong, L., Gong, T., Gradl, W., Gu, J. L., Escalante, A. G., Gui, L. C., Guo, F. K., Guo, J. C., Guo, J., Guo, Y. P., Guo, Z. H., Guskov, A., Han, K. L., Han, L., Han, M., Hao, X. Q., He, J. B., He, S. Q., He, X. G., He, Y. L., He, Z. B., Heng, Z. X., Hou, B. L., Hou, T. J., Hou, Y. R., Hu, C. Y., Hu, H. M., Hu, K., Hu, R. J., Hu, X. H., Hu, Y. C., Hua, J., Huang, G. S., Huang, J. S., Huang, M., Huang, Q. Y., Huang, W. Q., Huang, X. T., Huang, X. J., Huang, Y. B., Huang, Y. S., Hüsken, N., Ivanov, V., Ji, Q. P., Jia, J. J., Jia, S., Jia, Z. K., Jiang, H. B., Jiang, J., Jiang, S. Z., Jiao, J. B., Jiao, Z., Jing, H. J., Kang, X. L., Kang, X. S., Ke, B. C., Kenzie, M., Khoukaz, A., Koop, I., Kravchenko, E., Kuzmin, A., Lei, Y., Levichev, E., Li, C. H., Li, C., Li, D. Y., Li, F., Li, G., Li, H. B., Li, H., Li, H. N., Li, H. J., Li, H. L., Li, J. M., Li, J., Li, L., Li, L. Y., Li, N., Li, P. R., Li, R. H., Li, S., Li, T., Li, W. J., Li, X. H., Li, X. Q., Li, Y., Li, Y. Y., Li, Z. J., Liang, H., Liang, J. H., Liao, G. R., Liao, L. Z., Liao, Y., Lin, C. X., Lin, X. S., Liu, B. J., Liu, C. W., Liu, D., Liu, F., Liu, G. M., Liu, H. B., Liu, J., Liu, J. J., Liu, J. B., Liu, K., Liu, K. Y., Liu, L., Liu, Q., Liu, S. B., Liu, T., Liu, X., Liu, Y. W., Liu, Y., Liu, Y. L., Liu, Z. Q., Liu, Z. Y., Liu, Z. W., Logashenko, I., Long, Y., Lu, C. G., Lu, N., Lü, Q. F., Lu, Y., Lv, Z., Lukin, P., Luo, F. J., Luo, T., Luo, X. F., Lyu, H. J., Lyu, X. R., Ma, J. P., Ma, P., Ma, Y., Maas, F., Malde, S., Matvienko, D., Meng, Z. X., Mitchell, R., Dias, J. M., Nefediev, A., Nefedov, Y., Olsen, S. L., Ouyang, Q., Pakhlov, P., Pakhlova, G., Pan, X., Pan, Y., Passemar, E., Pei, Y. P., Peng, H. P., Peng, L., Peng, X. Y., Peng, X. J., Peters, K., Pivovarov, S., Pyata, E., Qi, B. B., Qi, Y. Q., Qian, W. B., Qian, Y., Qiao, C. F., Qin, J. J., Qin, L. Q., Qin, X. S., Qiu, T. L., Rademacker, J., Redmer, C. F., Sang, H. Y., Saur, M., Shan, W., Shan, X. Y., Shang, L. L., Shao, M., Shekhtman, L., Shen, C. P., Shen, J. M., Shen, Z. T., Shi, H. C., Shi, X. D., Shwartz, B., Sokolov, A., Song, J. J., Song, W. M., Song, Y., Song, Y. X., Sukharev, A., Sun, J. F., Sun, L., Sun, X. M., Sun, Y. J., Sun, Z. P., Tang, J., Tang, S. S., Tang, Z. B., Tian, C. H., Tian, J. S., Tikhonov, Y., Todyshev, K., Uglov, T., Vorobyev, V., Wan, B. D., Wang, B. L., Wang, B., Wang, D. Y., Wang, G. Y., Wang, G. L., Wang, H. L., Wang, J., Wang, J. H., Wang, J. C., Wang, M. L., Wang, R., Wang, S. B., Wang, W., Wang, W. P., Wang, X. C., Wang, X. D., Wang, X. L., Wang, X. P., Wang, X. F., Wang, Y. D., Wang, Y. P., Wang, Y. Q., Wang, Y. L., Wang, Y. G., Wang, Z. Y., Wang, Z. L., Wang, Z. G., Wei, D. H., Wei, X. L., Wei, X. M., Wen, Q. G., Wen, X. J., Wilkinson, G., Wu, B., Wu, J. J., Wu, L., Wu, P. W., Wu, T. W., Wu, Y. S., Xia, L., Xiang, T., Xiao, C. W., Xiao, D., Xiao, M., Xie, Y. H., Xing, Y., Xing, Z. Z., Xiong, X. N., Xu, F. R., Xu, J., Xu, L. L., Xu, Q. N., Xu, X. C., Xu, X. P., Xu, Y. C., Xu, Y. P., Xu, Y., Xu, Z. Z., Xuan, D. W., Xue, F. F., Yan, L., Yan, M. J., Yan, W. B., Yan, W. C., Yan, X. S., Yang, B. F., Yang, C., Yang, H. J., Yang, H. R., Yang, H. T., Yang, J. F., Yang, S. L., Yang, Y. D., Yang, Y. H., Yang, Y. S., Yang, Y. L., Yang, Z. Y., Yao, D. L., Yin, H., Yin, X. H., Yokozaki, N., You, S. Y., You, Z. Y., Yu, C. X., Yu, F. S., Yu, G. L., Yu, H. L., Yu, J. S., Yu, J. Q., Yuan, L., Yuan, X. B., Yue, Y. F., Zeng, M., Zeng, S., Zhang, A. L., Zhang, B. W., Zhang, G. Y., Zhang, G. Q., Zhang, H. J., Zhang, H. B., Zhang, J. Y., Zhang, J. L., Zhang, J., Zhang, L., Zhang, L. M., Zhang, R., Zhang, S. L., Zhang, T., Zhang, X., Zhang, Y., Zhang, Y. X., Zhang, Y. T., Zhang, Y. F., Zhang, Y. C., Zhang, Y. M., Zhang, Y. L., Zhang, Z. H., Zhang, Z. Y., Zhao, H. Y., Zhao, J., Zhao, L., Zhao, M. G., Zhao, Q., Zhao, R. G., Zhao, R. P., Zhao, Z. G., Zhao, Z. X., Zhemchugov, A., Zheng, B., Zheng, L., Zheng, Q. B., Zheng, R., Zheng, Y. H., Zhong, X. H., Zhou, H. J., Zhou, H. Q., Zhou, H., Zhou, S. H., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, Y. L., Zhou, Y., Zhou, Y. X., Zhou, Z. Y., Zhu, J. Y., Zhu, K., Zhu, R. D., Zhu, R. L., Zhu, S. H., Zhu, Y. C., Zhu, Z. A., Zhukova, V., Zhulanov, V., Zou, B. S., and Zuo, Y. B.
Subjects: High Energy Physics - Experiment, High Energy Physics - Phenomenology, Physics - Instrumentation and Detectors
Abstract: The Super $\tau$-Charm facility (STCF) is an electron-positron collider proposed by the Chinese particle physics community. It is designed to operate in a center-of-mass energy range from 2 to 7 GeV with a peak luminosity of $0.5\times 10^{35}{\rm cm}^{-2}{\rm s}^{-1}$ or higher. The STCF will produce a data sample about a factor of 100 larger than that by the present $\tau$-Charm factory -- the BEPCII, providing a unique platform for exploring the asymmetry of matter-antimatter (charge-parity violation), in-depth studies of the internal structure of hadrons and the nature of non-perturbative strong interactions, as well as searching for exotic hadrons and physics beyond the Standard Model. The STCF project in China is under development with an extensive R\&D program. This document presents the physics opportunities at the STCF, describes conceptual designs of the STCF detector system, and discusses future plans for detector R\&D and physics case studies.
Published: 2023
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15. Measurement of the $^{159}$Tb(n, $\gamma$) cross section at the CSNS Back-n facility

Author: Zhang, S., Li, G., Jiang, W., Wang, D. X., Ren, J., Li, E. T., Huang, M., Tang, J. Y., Ruan, X. C., Wang, H. W., Li, Z. H., Chen, Y. S., Liu, L. X., Li, X. X., Fan, Q. W., Fan, R. R., Hu, X. R., Wang, J. C., Li, X., Niu, 1D. D., Song, N., and Gu, M.
Subjects: Nuclear Experiment, Astrophysics - Solar and Stellar Astrophysics
Abstract: The stellar (n, $\gamma$) cross section data for the mass numbers around A $\approx$ 160 are of key importance to nucleosynthesis in the main component of the slow neutron capture process, which occur in the thermally pulsing asymptotic giant branch (TP--AGB). The new measurement of (n, $\gamma$) cross sections for $^{159}$Tb was performed using the C$_6$D$_6$ detector system at the back streaming white neutron beam line (Back-n) of the China spallation neutron source (CSNS) with neutron energies ranging from 1 eV to 1 MeV. Experimental resonance capture kernels were reported up to 1.2 keV neutron energy with this capture measurement. Maxwellian-averaged cross sections (MACS) were derived from the measured $^{159}$Tb (n, $\gamma$) cross sections at $kT$ = 5 $\sim$ 100 keV and are in good agreement with the recommended data of KADoNiS-v0.3 and JEFF-3.3, while KADoNiS-v1.0 and ENDF-VIII.0 significantly overestimate the present MACS up to 40$\%$ and 20$\%$, respectively. A sensitive test of the s-process nucleosynthesis was also performed with the stellar evolution code MESA. Significant changes in abundances around A $\approx$ 160 were observed between the ENDF/B-VIII.0 and present measured rate of $^{159}$Tb(n, $\gamma$)$^{160}$Tb in the MESA simulation., Comment: 13 pages, 7 figures
Published: 2022
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16. Monte-Carlo simulations on possible collimation effects of outflows to fan-beamed emission of ultraluminous accreting X-ray pulsars

Author: Hou, X., You, Y., Ji, L., Soria, R., Zhang, S. N., Ge, M. Y., Tao, L., Zhang, S., Feng, H., Zhou, M., Tuo, Y. L., Song, L. M., and Wang, J. C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Pulsating ultraluminous X-ray sources (PULXs) are accreting pulsars with apparent X-ray luminosity exceeding $10^{39}\, \rm erg\ s^{-1}$. We perform Monte-Carlo simulations to investigate whether high collimation effect (or strong beaming effect) is dominant in the presence of accretion outflows, for the fan beam emission of the accretion column of the neutron stars in PULXs. We show that the three nearby PULXs (RX J0209.6$-$7427, Swift J0243.6+6124 and SMC X-3), namely the three musketeers here, have their main pulsed emission not strongly collimated even if strong outflows exist. This conclusion can be extended to the current sample of extragalactic PULXs, if accretion outflows are commonly produced from them. This means that the observed high luminosity of PULXs is indeed intrinsic, which can be used to infer the existence of very strong surface magnetic fields of $\sim10^{13-14}$ G, possibly multipole fields. However, if strong outflows are launched from the accretion disks in PULXs as a consequence of disk spherization by radiation pressure, regular dipole magnetic fields of $\sim10^{12}$ G may be required, comparable to that of the three musketeers, which have experienced large luminosity changes from well below their Eddington limit ($2\times10^{38}\, \rm erg\ s^{-1}$ for a NS) to super-Eddington and their maximum luminosity fills the luminosity gap between Galactic pulsars and extragalactic PULXs., Comment: 26 pages, 8 figures, 1 table. Accepted by ApJ
Published: 2022
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17. Fan beamed X-ray emission from 1 keV to above 130 keV from the ultraluminous X-ray pulsar RX J0209.6-7427 in the Small Magellanic Cloud

Author: Hou, X., Ge, M. Y., Ji, L., Zhang, S. N., You, Y., Tao, L., Zhang, S., Soria, R., Feng, H., Zhou, M., Tuo, Y. L., Song, L. M., and Wang, J. C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present detailed timing and spectral analyses of the transient X-ray pulsar RX J0209.6$-$7427 in the Small Magellanic Cloud during its 2019 giant outburst. With a better known distance than most galactic X-ray pulsars, its peak luminosity is determined to be $(1.11\pm0.06)\times 10^{39}\, \rm erg\ s^{-1}$; it is thus a {\it bonda fide} pulsating ultraluminous X-ray source (PULX). Owing to the broad energy band of \textit{Insight}-HXMT, its pulsed X-ray emission was detected from 1 keV up to the 130$-$180 keV band, which is the highest energy emission detected from any PULXs outside the Milky Way. This allows us to conclude that its main pulsed X-ray emission is from the "fan beam" of the accretion column, and its luminosity is thus intrinsic. We also estimate its magnetic field of (4.8$-$8.6)$\times10^{12}$ G or (1.7$-$2.2)$\times10^{13}$ G, from its spin evolution or transition in the accretion column structure during the outburst; we suggest that the two values of the magnetic field strength correspond to the dipole and multipole magnetic fields of the neutron star, similar to the recent discovery in the Galactic PULX Swift J0243.6+6124. Therefore, the nature of the neutron star and its ULX emission can be understood within the current theoretical frame of accreting neutron stars. This may have implications for understanding the nature of those farther away extragalactic PULXs., Comment: 31 pages, 14 figures, 5 tables. Accepted by ApJ
Published: 2022

18. Flux Variations of Cosmic Ray Air Showers Detected by LHAASO-KM2A During a Thunderstorm on 10 June 2021

Author: LHAASO Collaboration, Aharonian, F., An, Q., Axikegu, Bai, L. X., Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, J. T., Cao, Zhe, Cao, Zhen, Chang, J., Chang, J. F., Chen, E. S., Chen, Liang, Chen, Long, Chen, M. J., Chen, M. L., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, X. J., Chen, Y., Cheng, H. L., Cheng, N., Cheng, Y. D., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, della Volpe, D., Duan, K. K., Fan, J. H., Fan, Y. Z., Fan, Z. X., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, X. T., Feng, Y. L., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Gong, G. H., Gou, Q. B., Gu, M. H., Gu, F. L., Guo, J. G., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, S. L., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S., Hu, S. C., Hu, X. J., Huang, D. H., Huang, W. H., Huang, X. T., Huang, X. Y., Huang, Y., Huang, Z. C., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, Z. J., Jin, M., Kang, M. M., Ke, T., Kuleshov, D., Li, B. B., Li, Cheng, Li, Cong, Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, Jian, Li, Jie, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. S., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Long, W. J., Lu, R., Luo, Q., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Masood, A., Min, Z., Mitthumsiri, W., Nan, Y. C., Ou, Z. W., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Sáiz, A., Shao, C. Y., Shao, L., Shchegolev, O., Sheng, X. D., Shi, J. Y., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Z. B., Tian, W. W., Wang, B. D., Wang, C., Wang, H., Wang, H. G., Wang, J. C., Wang, J. S., Wang, L. P., Wang, L. Y., Wang, R., Wang, R. N., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Y. P., Wang, Z. H. Wang. Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, X. F., W, Y. S., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, G. G., Xin, Y. L., Xing, Y., Xiong, Z., Xu, D. L., Xu, R. X., Xue, L., Yan, D. H., Yan, J. Z., Yang, C. W., Yang, F. F., Yang, H. W., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zeng, Z. K., Zha, M., Zhai, X. X., Zhang, B. B., Zhang, F., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, L. X., Zhang, Li, Zhang, Lu, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Y. L., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zheng, Y., Zhou, B., Zhou, H., Zhou, J. N., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo, X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract: The Large High Altitude Air Shower Observatory (LHAASO) has three sub-arrays, KM2A, WCDA and WFCTA. The flux variations of cosmic ray air showers were studied by analyzing the KM2A data during the thunderstorm on 10 June 2021. The number of shower events that meet the trigger conditions increases significantly in atmospheric electric fields, with maximum fractional increase of 20%. The variations of trigger rates (increases or decreases) are found to be strongly dependent on the primary zenith angle. The flux of secondary particles increases significantly, following a similar trend with that of the shower events. To better understand the observed behavior, Monte Carlo simulations are performed with CORSIKA and G4KM2A (a code based on GEANT4). We find that the experimental data (in saturated negative fields) are in good agreement with simulations, assuming the presence of a uniform upward electric field of 700 V/cm with a thickness of 1500 m in the atmosphere above the observation level. Due to the acceleration/deceleration and deflection by the atmospheric electric field, the number of secondary particles with energy above the detector threshold is modified, resulting in the changes in shower detection rate., Comment: 18 pages, 11 figures
Published: 2022
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19. STCF conceptual design report (Volume 1): Physics & detector

Author: Achasov, M., Ai, X. C., An, L. P., Aliberti, R., An, Q., Bai, X. Z., Bai, Y., Bakina, O., Barnyakov, A., Blinov, V., Bobrovnikov, V., Bodrov, D., Bogomyagkov, A., Bondar, A., Boyko, I., Bu, Z. H., Cai, F. M., Cai, H., Cao, J. J., Cao, Q. H., Cao, X., Cao, Z., Chang, Q., Chao, K. T., Chen, D. Y., Chen, H., Chen, H. X., Chen, J. F., Chen, K., Chen, L. L., Chen, P., Chen, S. L., Chen, S. M., Chen, S., Chen, S. P., Chen, W., Chen, X., Chen, X. F., Chen, X. R., Chen, Y., Chen, Y. Q., Cheng, H. Y., Cheng, J., Cheng, S., Cheng, T. G., Dai, J. P., Dai, L. Y., Dai, X. C., Dedovich, D., Denig, A., Denisenko, I., Dias, J. M., Ding, D. Z., Dong, L. Y., Dong, W. H., Druzhinin, V., Du, D. S., Du, Y. J., Du, Z. G., Duan, L. M., Epifanov, D., Fan, Y. L., Fang, S. S., Fang, Z. J., Fedotovich, G., Feng, C. Q., Feng, X., Feng, Y. T., Fu, J. L., Gao, J., Gao, Y. N., Ge, P. S., Geng, C. Q., Geng, L. S., Gilman, A., Gong, L., Gong, T., Gou, B., Gradl, W., Gu, J. L., Guevara, A., Gui, L. C., Guo, A. Q., Guo, F. K., Guo, J. C., Guo, J., Guo, Y. P., Guo, Z. H., Guskov, A., Han, K. L., Han, L., Han, M., Hao, X. Q., He, J. B., He, S. Q., He, X. G., He, Y. L., He, Z. B., Heng, Z. X., Hou, B. L., Hou, T. J., Hou, Y. R., Hu, C. Y., Hu, H. M., Hu, K., Hu, R. J., Hu, W. H., Hu, X. H., Hu, Y. C., Hua, J., Huang, G. S., Huang, J. S., Huang, M., Huang, Q. Y., Huang, W. Q., Huang, X. T., Huang, X. J., Huang, Y. B., Huang, Y. S., Hüsken, N., Ivanov, V., Ji, Q. P., Jia, J. J., Jia, S., Jia, Z. K., Jiang, H. B., Jiang, J., Jiang, S. Z., Jiao, J. B., Jiao, Z., Jing, H. J., Kang, X. L., Kang, X. S., Ke, B. C., Kenzie, M., Khoukaz, A., Koop, I., Kravchenko, E., Kuzmin, A., Lei, Y., Levichev, E., Li, C. H., Li, C., Li, D. Y., Li, F., Li, G., Li, G., Li, H. B., Li, H., Li, H. N., Li, H. J., Li, H. L., Li, J. M., Li, J., Li, L., Li, L., Li, L. Y., Li, N., Li, P. R., Li, R. H., Li, S., Li, T., Li, W. J., Li, X., Li, X. H., Li, X. Q., Li, X. H., Li, Y., Li, Y. Y., Li, Z. J., Liang, H., Liang, J. H., Liang, Y. T., Liao, G. R., Liao, L. Z., Liao, Y., Lin, C. X., Lin, D. X., Lin, X. S., Liu, B. J., Liu, C. W., Liu, D., Liu, F., Liu, G. M., Liu, H. B., Liu, J., Liu, J. J., Liu, J. B., Liu, K., Liu, K. Y., Liu, K., Liu, L., Liu, Q., Liu, S. B., Liu, T., Liu, X., Liu, Y. W., Liu, Y., Liu, Y. L., Liu, Z. Q., Liu, Z. Y., Liu, Z. W., Logashenko, I., Long, Y., Lu, C. G., Lu, J. X., Lu, N., Lü, Q. F., Lu, Y., Lu, Y., Lu, Z., Lukin, P., Luo, F. J., Luo, T., Luo, X. F., Lyu, H. J., Lyu, X. R., Ma, J. P., Ma, P., Ma, Y., Ma, Y. M., Maas, F., Malde, S., Matvienko, D., Meng, Z. X., Mitchell, R., Nefediev, A., Nefedov, Y., Olsen, S. L., Ouyang, Q., Pakhlov, P., Pakhlova, G., Pan, X., Pan, Y., Passemar, E., Pei, Y. P., Peng, H. P., Peng, L., Peng, X. Y., Peng, X. J., Peters, K., Pivovarov, S., Pyata, E., Qi, B. B., Qi, Y. Q., Qian, W. B., Qian, Y., Qiao, C. F., Qin, J. J., Qin, J. J., Qin, L. Q., Qin, X. S., Qiu, T. L., Rademacker, J., Redmer, C. F., Sang, H. Y., Saur, M., Shan, W., Shan, X. Y., Shang, L. L., Shao, M., Shekhtman, L., Shen, C. P., Shen, J. M., Shen, Z. T., Shi, H. C., Shi, X. D., Shwartz, B., Sokolov, A., Song, J. J., Song, W. M., Song, Y., Song, Y. X., Sukharev, A., Sun, J. F., Sun, L., Sun, X. M., Sun, Y. J., Sun, Z. P., Tang, J., Tang, S. S., Tang, Z. B., Tian, C. H., Tian, J. S., Tian, Y., Tikhonov, Y., Todyshev, K., Uglov, T., Vorobyev, V., Wan, B. D., Wang, B. L., Wang, B., Wang, D. Y., Wang, G. Y., Wang, G. L., Wang, H. L., Wang, J., Wang, J. H., Wang, J. C., Wang, M. L., Wang, R., Wang, R., Wang, S. B., Wang, W., Wang, W. P., Wang, X. C., Wang, X. D., Wang, X. L., Wang, X. L., Wang, X. P., Wang, X. F., Wang, Y. D., Wang, Y. P., Wang, Y. Q., Wang, Y. L., Wang, Y. G., Wang, Z. Y., Wang, Z. Y., Wang, Z. L., Wang, Z. G., Wei, D. H., Wei, X. L., Wei, X. M., Wen, Q. G., Wen, X. J., Wilkinson, G., Wu, B., Wu, J. J., Wu, L., Wu, P., Wu, T. W., Wu, Y. S., Xia, L., Xiang, T., Xiao, C. W., Xiao, D., Xiao, M., Xie, K. P., Xie, Y. H., Xing, Y., Xing, Z. Z., Xiong, X. N., Xu, F. R., Xu, J., Xu, L. L., Xu, Q. N., Xu, X. C., Xu, X. P., Xu, Y. C., Xu, Y. P., Xu, Y., Xu, Z. Z., Xuan, D. W., Xue, F. F., Yan, L., Yan, M. J., Yan, W. B., Yan, W. C., Yan, X. S., Yang, B. F., Yang, C., Yang, H. J., Yang, H. R., Yang, H. T., Yang, J. F., Yang, S. L., Yang, Y. D., Yang, Y. H., Yang, Y. S., Yang, Y. L., Yang, Z. W., Yang, Z. Y., Yao, D. L., Yin, H., Yin, X. H., Yokozaki, N., You, S. Y., You, Z. Y., Yu, C. X., Yu, F. S., Yu, G. L., Yu, H. L., Yu, J. S., Yu, J. Q., Yuan, L., Yuan, X. B., Yuan, Z. Y., Yue, Y. F., Zeng, M., Zeng, S., Zhang, A. L., Zhang, B. W., Zhang, G. Y., Zhang, G. Q., Zhang, H. J., Zhang, H. B., Zhang, J. Y., Zhang, J. L., Zhang, J., Zhang, L., Zhang, L. M., Zhang, Q. A., Zhang, R., Zhang, S. L., Zhang, T., Zhang, X., Zhang, Y., Zhang, Y. J., Zhang, Y. X., Zhang, Y. T., Zhang, Y. F., Zhang, Y. C., Zhang, Y., Zhang, Y., Zhang, Y. M., Zhang, Y. L., Zhang, Z. H., Zhang, Z. Y., Zhang, Z. Y., Zhao, H. Y., Zhao, J., Zhao, L., Zhao, M. G., Zhao, Q., Zhao, R. G., Zhao, R. P., Zhao, Y. X., Zhao, Z. G., Zhao, Z. X., Zhemchugov, A., Zheng, B., Zheng, L., Zheng, Q. B., Zheng, R., Zheng, Y. H., Zhong, X. H., Zhou, H. J., Zhou, H. Q., Zhou, H., Zhou, S. H., Zhou, X., Zhou, X. K., Zhou, X. P., Zhou, X. R., Zhou, Y. L., Zhou, Y., Zhou, Y. X., Zhou, Z. Y., Zhu, J. Y., Zhu, K., Zhu, R. D., Zhu, R. L., Zhu, S. H., Zhu, Y. C., Zhu, Z. A., Zhukova, V., Zhulanov, V., Zou, B. S., and Zuo, Y. B.
Published: 2024
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20. An Infrared Temperature Measurement Method for Hot Stamping Parts Considering Directional Emissivity

Author: Gu, Y. K., Zhao, Z. H., Wang, J. C., Min, J. Y., Lin, J. P., He, P. X., Shi, L. Y., Wang, R. L., Xiao, Shengxiong, Editor-in-Chief, Bassir, David, Series Editor, Gao, Bingbing, Series Editor, Jiang, Yongchao, Series Editor, Li, Jia, Series Editor, Mazumdar, Sayantan, Series Editor, Sun, Qijun, Series Editor, Tang, Juntao, Series Editor, Xiong, Chuanyin, Series Editor, Xu, Hexiu, Series Editor, Yang, Jun, Series Editor, Zhang, Yisheng, editor, and Ma, Mingtu, editor
Published: 2023
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21. Reconstruction of Cherenkov image by multiple telescopes of LHAASO-WFCTA

Author: Aharonian, F., An, Q., Axikegu, Bai, L. X., Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, J. T., Cao, Zhe, Cao, Zhen, Chang, J., Chang, J. F., Chen, E. S., Chen, Liang, Chen, Liang, Chen, Long, Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, Y., Cheng, H. L., Cheng, N., Cheng, Y. D., Cui, S. W., Cui, X. H., Cui, Y. D., D’Ettorre Piazzoli, B., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, della Volpe, D., Duan, K. K., Fan, J. H., Fan, Y. Z., Fan, Z. X., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, X. T., Feng, Y. L., Gao, B., Gao, C. D., Gao, L. Q., Gao, Q., Gao, W., Gao, W. K., Ge, M. M., Geng, L. S., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, F. L., Guo, J. G., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, S. L., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, C., Hou, X., Hu, H. B., Hu, Q., Hu, S., Hu, S. C., Hu, X. J., Huang, D. H., Huang, W. H., Huang, X. T., Huang, X. Y., Huang, Y., Huang, Z. C., Ji, X. L., Jia, H. Y., Jia, K., Jiang, K., Jiang, Z. J., Jin, M., Kang, M. M., Ke, T., Kuleshov, D., Levochkin, K., Li, B. B., Li, Cheng, Li, Cong, Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, Jian, Li, Jie, Li, K., Li, W. L., Li, X. R., Li, Xin, Li, Xin, Li, Y. Z., Li, Zhe, Li, Zhuo, Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. S., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y., Liu, Y. N., Long, W. J., Lu, R., Luo, Q., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Masood, A., Min, Z., Mitthumsiri, W., Nan, Y. C., Ou, Z. W., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Qi, Y. Q., Qiao, B. Q., Qin, J. J., Ruffolo, D., Sáiz, A., Shao, C. Y., Shao, L., Shchegolev, O., Sheng, X. D., Shi, J. Y., Song, H. C., Stenkin, Yu. V., Stepanov, V., Su, Y., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Z. B., Tian, W. W., Wang, B. D., Wang, C., Wang, H., Wang, H. G., Wang, J. C., Wang, J. S., Wang, L. P., Wang, L. Y., Wang, R., Wang, R. N., Wang, W., Wang, X. G., Wang, X. Y., Wang, Y., Wang, Y. D., Wang, Y. J., Wang, Y. P., Wang, Z. H., Wang, Z. X., Wang, Zhen, Wang, Zheng, Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, X. F., Wu, Y. S., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, D. X., Xiao, G., Xin, G. G., Xin, Y. L., Xing, Y., Xiong, Z., Xu, D. L., Xu, R. X., Xue, L., Yan, D. H., Yan, J. Z., Yang, C. W., Yang, F. F., Yang, H. W., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Yue, H., Zeng, H. D., Zeng, T. X., Zeng, W., Zeng, Z. K., Zha, M., Zhai, X. X., Zhang, B. B., Zhang, F., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, L. X., Zhang, Li, Zhang, Lu, Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. B., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y. F., Zhang, Y. L., Zhang, Yi, Zhang, Yong, Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zheng, Y., Zhou, B., Zhou, H., Zhou, J. N., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo, X.
Published: 2022
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22. Study on Drilling of Additively Manufactured Inconel 718

Author: Sivaraman, V., Nagesha, B. K., Wang, J. C., Cavas-Martínez, Francisco, Series Editor, Chaari, Fakher, Series Editor, di Mare, Francesca, Series Editor, Gherardini, Francesco, Series Editor, Haddar, Mohamed, Series Editor, Ivanov, Vitalii, Series Editor, Kwon, Young W., Series Editor, Trojanowska, Justyna, Series Editor, Krishnapillai, Shankar, editor, R., Velmurugan, editor, and Ha, Sung Kyu, editor
Published: 2022
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23. High-Strength Headed Bars in Joints of Special Moment Frames under Cyclic Loading.

Author: Lee, H.-J., Yu, F.-C., Lin, K.-C., Wang, J.-C., Worsfold, B. L., and Silva, J. F.
Subjects: CYCLIC loads, BEAM-column joints, TRANSVERSE reinforcements, MINERAL aggregate testing, SEISMIC response, CONCRETE joints
Abstract: This paper presents cyclic test results of nine beam-column joints, fabricated with Grades 60, 80, and 100 (Grades 420, 550, and 690) No. 11 (D36) headed bars in joints with matching concrete strengths. With the exception of the joint shear determination, each specimen was designed in accordance with ACI 318-14 provisions for special moment frame joints. The headed bar embedment length was determined using 1.0fy in accordance with ACI 318-14, rather than the ACI 318-19 requirement to use 1.25fy to calculate the development length. Test results demonstrate that the ACI 318-14 development length can be used for closely spaced high-strength No. 11 (D36) headed bars in joints with Code-conforming transverse reinforcement. This paper also aggregates the test data with prior research and compares the data with descriptive equations and breakout methodology for assessing the development length and anchorage strength of headed bars. The results support several design recommendations for the ACI 318 provisions. [ABSTRACT FROM AUTHOR]
Published: 2024
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24. Comprehensive analysis of the PD-L1 and immune infiltrates of N6-methyladenosine related long non-coding RNAs in bladder cancer

Author: Xue, M. Q., Wang, Y. L., Wang, J. C., Wang, X. D., Wang, X. J., and Zhang, Y. Q.
Published: 2022
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25. Line-of-shower trigger method to lower energy threshold for GRB detection using LHAASO-WCDA

Author: Aharonian, F., An, Q., Axikegu, Bai, L. X., Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, H., Cai, J. T., Cao, Z., Cao, Z., Chang, J., Chang, J. F., Chang, X. C., Chen, B. M., Chen, J., Chen, L., Chen, L., Chen, L., Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, X. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, Volpe, D. della, Piazzoli, B. D’Ettorre, Dong, X. J., Fan, J. H., Fan, Y. Z., Fan, Z. X., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, Y. L., Gao, B., Gao, C. D., Gao, Q., Gao, W., Ge, M. M., Geng, L. S., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, J. G., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. C., He, S. L., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, C., Hou, X., Hu, H. B., Hu, S., Hu, S. C., Hu, X. J., Huang, D. H., Huang, Q. L., Huang, W. H., Huang, X. T., Huang, Z. C., Ji, F., Ji, X. L., Jia, H. Y., Jiang, K., Jiang, Z. J., Jin, C., Kuleshov, D., Levochkin, K., Li, B. B., Li, C., Li, C., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, K., Li, W. L., Li, X., Li, X., Li, X. R., Li, Y., Li, Y. Z., Li, Z., Li, Z., Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. S., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y. N., Liu, Z. X., Long, W. J., Lu, R., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Masood, A., Mitthumsiri, W., Montaruli, T., Nan, Y. C., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Ruffolo, D., Rulev, V., Sáiz, A., Shao, L., Shchegolev, O., Sheng, X. D., Shi, J. R., Song, H. C., Stenkin, Yu. V., Stepanov, V., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Z. B., Tian, W. W., Wang, B. D., Wang, C., Wang, H., Wang, H. G., Wang, J. C., Wang, J. S., Wang, L. P., Wang, L. Y., Wang, R. N., Wang, W., Wang, W., Wang, X. G., Wang, X. J., Wang, X. Y., Wang, Y. D., Wang, Y. J., Wang, Y. P., Wang, Z., Wang, Z., Wang, Z. H., Wang, Z. X., Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, W. X., Wu, X. F., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, G., Xiao, H. B., Xin, G. G., Xin, Y. L., Xing, Y., Xu, D. L., Xu, R. X., Xue, L., Yan, D. H., Yang, C. W., Yang, F. F., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Zeng, H. D., Zeng, T. X., Zeng, W., Zeng, Z. K., Zha, M., Zhai, X. X., Zhang, B. B., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, J. W., Zhang, L., Zhang, L., Zhang, L. X., Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y., Zhang, Y., Zhang, Y. F., Zhang, Y. L., Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zheng, Y., Zhou, B., Zhou, H., Zhou, J. N., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo, X.
Published: 2021
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26. A dynamic range extension system for LHAASO WCDA-1

Author: Aharonian, F., An, Q., Axikegu, Bai, L. X., Bai, Y. X., Bao, Y. W., Bastieri, D., Bi, X. J., Bi, Y. J., Cai, H., Cai, J. T., Cao, Z., Cao, Z., Chang, J., Chang, J. F., Chang, X. C., Chen, B. M., Chen, J., Chen, L., Chen, L., Chen, L., Chen, M. J., Chen, M. L., Chen, Q. H., Chen, S. H., Chen, S. Z., Chen, T. L., Chen, X. L., Chen, Y., Cheng, N., Cheng, Y. D., Cui, S. W., Cui, X. H., Cui, Y. D., Dai, B. Z., Dai, H. L., Dai, Z. G., Danzengluobu, Volpe, D. della, Piazzoli, B. D’Ettorre, Dong, X. J., Fan, J. H., Fan, Y. Z., Fan, Z. X., Fang, J., Fang, K., Feng, C. F., Feng, L., Feng, S. H., Feng, Y. L., Gao, B., Gao, C. D., Gao, Q., Gao, W., Ge, M. M., Geng, L. S., Gong, G. H., Gou, Q. B., Gu, M. H., Guo, J. G., Guo, X. L., Guo, Y. Q., Guo, Y. Y., Han, Y. A., He, H. H., He, H. N., He, J. C., He, S. L., He, X. B., He, Y., Heller, M., Hor, Y. K., Hou, C., Hou, X., Hu, H. B., Hu, S., Hu, S. C., Hu, X. J., Huang, D. H., Huang, Q. L., Huang, W. H., Huang, X. T., Huang, Y., Huang, Z. C., Ji, F., Ji, X. L., Jia, H. Y., Jiang, K., Jiang, Z. J., Jin, C., Kuleshov, D., Levochkin, K., Li, B. B., Li, C., Li, C., Li, F., Li, H. B., Li, H. C., Li, H. Y., Li, J., Li, K., Li, W. L., Li, X., Li, X., Li, X. R., Li, Y., Li, Y. Z., Li, Z., Li, Z., Liang, E. W., Liang, Y. F., Lin, S. J., Liu, B., Liu, C., Liu, D., Liu, H., Liu, H. D., Liu, J., Liu, J. L., Liu, J. S., Liu, J. Y., Liu, M. Y., Liu, R. Y., Liu, S. M., Liu, W., Liu, Y. N., Liu, Z. X., Long, W. J., Lu, R., Lv, H. K., Ma, B. Q., Ma, L. L., Ma, X. H., Mao, J. R., Masood, A., Mitthumsiri, W., Montaruli, T., Nan, Y. C., Pang, B. Y., Pattarakijwanich, P., Pei, Z. Y., Qi, M. Y., Ruffolo, D., Rulev, V., Sáiz, A., Shao, L., Shchegolev, O., Sheng, X. D., Shi, J. R., Song, H. C., Stenkin, Yu. V., Stepanov, V., Sun, Q. N., Sun, X. N., Sun, Z. B., Tam, P. H. T., Tang, Z. B., Tian, W. W., Wang, B. D., Wang, C., Wang, H., Wang, H. G., Wang, J. C., Wang, J. S., Wang, L. P., Wang, L. Y., Wang, R. N., Wang, W., Wang, W., Wang, X. G., Wang, X. J., Wang, X. Y., Wang, Y. D., Wang, Y. J., Wang, Y. P., Wang, Z., Wang, Z., Wang, Z. H., Wang, Z. X., Wei, D. M., Wei, J. J., Wei, Y. J., Wen, T., Wu, C. Y., Wu, H. R., Wu, S., Wu, W. X., Wu, X. F., Xi, S. Q., Xia, J., Xia, J. J., Xiang, G. M., Xiao, G., Xiao, H. B., Xin, G. G., Xin, Y. L., Xing, Y., Xu, D. L., Xu, R. X., Xue, L., Yan, D. H., Yang, C. W., Yang, F. F., Yang, J. Y., Yang, L. L., Yang, M. J., Yang, R. Z., Yang, S. B., Yao, Y. H., Yao, Z. G., Ye, Y. M., Yin, L. Q., Yin, N., You, X. H., You, Z. Y., Yu, Y. H., Yuan, Q., Zeng, H. D., Zeng, T. X., Zeng, W., Zeng, Z. K., Zha, M., Zhai, X. X., Zhang, B. B., Zhang, H. M., Zhang, H. Y., Zhang, J. L., Zhang, J. W., Zhang, L., Zhang, L., Zhang, L. X., Zhang, P. F., Zhang, P. P., Zhang, R., Zhang, S. R., Zhang, S. S., Zhang, X., Zhang, X. P., Zhang, Y., Zhang, Y., Zhang, Y. F., Zhang, Y. L., Zhao, B., Zhao, J., Zhao, L., Zhao, L. Z., Zhao, S. P., Zheng, F., Zheng, Y., Zhou, B., Zhou, H., Zhou, J. N., Zhou, P., Zhou, R., Zhou, X. X., Zhu, C. G., Zhu, F. R., Zhu, H., Zhu, K. J., and Zuo, X.
Published: 2021
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27. Advances in additively manufactured titanium alloys by powder bed fusion and directed energy deposition: Microstructure, defects, and mechanical behavior

Author: Ma, Hongyi Y., Wang, J. C., Qin, Peng, Liu, Y. J., Chen, L. Y., Wang, L. Q., Zhang, Laichang, Ma, Hongyi Y., Wang, J. C., Qin, Peng, Liu, Y. J., Chen, L. Y., Wang, L. Q., and Zhang, Laichang
Abstract: Ti and its alloys have been broadly adopted across various industries owing to their outstanding properties, such as high strength-to-weight ratio, excellent fatigue performance, exceptional corrosion resistance and so on. Additive manufacturing (AM) is a complement to, rather than a replacement for, traditional manufacturing processes. It enhances flexibility in fabricating complex components and resolves machining challenges, resulting in reduced lead times for custom designs. However, owing to distinctions among various AM technologies, Ti alloys fabricated by different AM methods usually present differences in microstructure and defects, which can significantly influence the mechanical performance of built parts. Therefore, having an in-depth knowledge of the scientific aspects of fabrication and material properties is crucial to achieving high-performance Ti alloys through different AM methods. This article reviews the mechanical properties of Ti alloys fabricated by two mainstream powder-type AM techniques: powder bed fusion (PBF) and directed energy deposition (DED). The review examines several key aspects, encompassing phase formation, grain size and morphology, and defects, and provides an in-depth analysis of their influence on the mechanical behaviors of Ti alloys. This review can aid researchers and engineers in selecting appropriate PBF or DED methods and optimizing their process parameters to fabricate high-performance Ti alloys for a wide range of industrial applications.
Published: 2024

28. Atypical Site of Presentation of a Rare Type of SMARCA4-Positive Cutaneous Squamous Cell Carcinoma of the Skin: Case Report and Review of the Literature.

Author: Yadav, Ruchi, Din, Shaun, Moussaris, Harry, Yadav, Vivek, Raman, Shakthi, Gandhi, Anjula, Avezbakiyev, Boris, and Wang, J. C.
Abstract: Cutaneous squamous cell carcinoma (cSCC) comprises 20% of cases of nonmelanoma skin cancers in the United States. In total, 3% to 5% of squamous cell carcinoma (SCC) are metastatic at the time of presentation, associated with significant mortality due to a lack of standardized treatment options. In total, 95% of these tumors are amenable to the initial standard of treatment, which is surgical resection. However, a small percentage of them require systemic therapy as they are either locally advanced to regional lymph nodes or have distant metastasis. The common sites of presentation of cSCC are the scalp and the face with predictable spread to the intra-parotid, upper jugular, and perifacial lymph nodes. In our case report, however, our patient had a large lump lesion on the upper back, an unusual site of presentation of cSCC, with locally advanced metastasis to the left axillary lymph nodes. Subsequently, the tumor marker study revealed a positive SMARCA4 variant (the essential ATPase subunit of the Switch (SWI)/Sucrose Nonfermenting (SNF) chromatin-remodeling complex) that is even rarer in the context of cSCC. Furthermore, abnormalities in SWI/SNF chromatin-remodeling complex subunits have shown promising results as a target therapy for immune checkpoint inhibitor (ICI) therapy. We present an atypical presentation site of locally advanced rare variant SMARCA4-positive cSCC in a patient who received treatment with chemoradiation and systemic therapy with ICI after primary surgical resection. To date, only 2 cases of SMARCA4-positive cSCC were found in the literature with no details of the treatment received. Our case is unique in its atypical site of presentation as well as showing partial response to radiotherapy (RT) and systemic therapy with ICI. [ABSTRACT FROM AUTHOR]
Published: 2024
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29. STCF conceptual design report (Volume 1): Physics & detector

Author: Achasov, M., primary, Ai, X. C., additional, An, L. P., additional, Aliberti, R., additional, An, Q., additional, Bai, X. Z., additional, Bai, Y., additional, Bakina, O., additional, Barnyakov, A., additional, Blinov, V., additional, Bobrovnikov, V., additional, Bodrov, D., additional, Bogomyagkov, A., additional, Bondar, A., additional, Boyko, I., additional, Bu, Z. H., additional, Cai, F. M., additional, Cai, H., additional, Cao, J. J., additional, Cao, Q. H., additional, Cao, X., additional, Cao, Z., additional, Chang, Q., additional, Chao, K. T., additional, Chen, D. Y., additional, Chen, H., additional, Chen, H. X., additional, Chen, J. F., additional, Chen, K., additional, Chen, L. L., additional, Chen, P., additional, Chen, S. L., additional, Chen, S. M., additional, Chen, S., additional, Chen, S. P., additional, Chen, W., additional, Chen, X., additional, Chen, X. F., additional, Chen, X. R., additional, Chen, Y., additional, Chen, Y. Q., additional, Cheng, H. Y., additional, Cheng, J., additional, Cheng, S., additional, Cheng, T. G., additional, Dai, J. P., additional, Dai, L. Y., additional, Dai, X. C., additional, Dedovich, D., additional, Denig, A., additional, Denisenko, I., additional, Dias, J. M., additional, Ding, D. Z., additional, Dong, L. Y., additional, Dong, W. H., additional, Druzhinin, V., additional, Du, D. S., additional, Du, Y. J., additional, Du, Z. G., additional, Duan, L. M., additional, Epifanov, D., additional, Fan, Y. L., additional, Fang, S. S., additional, Fang, Z. J., additional, Fedotovich, G., additional, Feng, C. Q., additional, Feng, X., additional, Feng, Y. T., additional, Fu, J. L., additional, Gao, J., additional, Gao, Y. N., additional, Ge, P. S., additional, Geng, C. Q., additional, Geng, L. S., additional, Gilman, A., additional, Gong, L., additional, Gong, T., additional, Gou, B., additional, Gradl, W., additional, Gu, J. L., additional, Guevara, A., additional, Gui, L. C., additional, Guo, A. Q., additional, Guo, F. K., additional, Guo, J. C., additional, Guo, J., additional, Guo, Y. P., additional, Guo, Z. H., additional, Guskov, A., additional, Han, K. L., additional, Han, L., additional, Han, M., additional, Hao, X. Q., additional, He, J. B., additional, He, S. Q., additional, He, X. G., additional, He, Y. L., additional, He, Z. B., additional, Heng, Z. X., additional, Hou, B. L., additional, Hou, T. J., additional, Hou, Y. R., additional, Hu, C. Y., additional, Hu, H. M., additional, Hu, K., additional, Hu, R. J., additional, Hu, W. H., additional, Hu, X. H., additional, Hu, Y. C., additional, Hua, J., additional, Huang, G. S., additional, Huang, J. S., additional, Huang, M., additional, Huang, Q. Y., additional, Huang, W. Q., additional, Huang, X. T., additional, Huang, X. J., additional, Huang, Y. B., additional, Huang, Y. S., additional, Hüsken, N., additional, Ivanov, V., additional, Ji, Q. P., additional, Jia, J. J., additional, Jia, S., additional, Jia, Z. K., additional, Jiang, H. B., additional, Jiang, J., additional, Jiang, S. Z., additional, Jiao, J. B., additional, Jiao, Z., additional, Jing, H. J., additional, Kang, X. L., additional, Kang, X. S., additional, Ke, B. C., additional, Kenzie, M., additional, Khoukaz, A., additional, Koop, I., additional, Kravchenko, E., additional, Kuzmin, A., additional, Lei, Y., additional, Levichev, E., additional, Li, C. H., additional, Li, C., additional, Li, D. Y., additional, Li, F., additional, Li, G., additional, Li, H. B., additional, Li, H., additional, Li, H. N., additional, Li, H. J., additional, Li, H. L., additional, Li, J. M., additional, Li, J., additional, Li, L., additional, Li, L. Y., additional, Li, N., additional, Li, P. R., additional, Li, R. H., additional, Li, S., additional, Li, T., additional, Li, W. J., additional, Li, X., additional, Li, X. H., additional, Li, X. Q., additional, Li, Y., additional, Li, Y. Y., additional, Li, Z. J., additional, Liang, H., additional, Liang, J. H., additional, Liang, Y. T., additional, Liao, G. R., additional, Liao, L. Z., additional, Liao, Y., additional, Lin, C. X., additional, Lin, D. X., additional, Lin, X. S., additional, Liu, B. J., additional, Liu, C. W., additional, Liu, D., additional, Liu, F., additional, Liu, G. M., additional, Liu, H. B., additional, Liu, J., additional, Liu, J. J., additional, Liu, J. B., additional, Liu, K., additional, Liu, K. Y., additional, Liu, L., additional, Liu, Q., additional, Liu, S. B., additional, Liu, T., additional, Liu, X., additional, Liu, Y. W., additional, Liu, Y., additional, Liu, Y. L., additional, Liu, Z. Q., additional, Liu, Z. Y., additional, Liu, Z. W., additional, Logashenko, I., additional, Long, Y., additional, Lu, C. G., additional, Lu, J. X., additional, Lu, N., additional, Lü, Q. F., additional, Lu, Y., additional, Lu, Z., additional, Lukin, P., additional, Luo, F. J., additional, Luo, T., additional, Luo, X. F., additional, Lyu, H. J., additional, Lyu, X. R., additional, Ma, J. P., additional, Ma, P., additional, Ma, Y., additional, Ma, Y. M., additional, Maas, F., additional, Malde, S., additional, Matvienko, D., additional, Meng, Z. X., additional, Mitchell, R., additional, Nefediev, A., additional, Nefedov, Y., additional, Olsen, S. L., additional, Ouyang, Q., additional, Pakhlov, P., additional, Pakhlova, G., additional, Pan, X., additional, Pan, Y., additional, Passemar, E., additional, Pei, Y. P., additional, Peng, H. P., additional, Peng, L., additional, Peng, X. Y., additional, Peng, X. J., additional, Peters, K., additional, Pivovarov, S., additional, Pyata, E., additional, Qi, B. B., additional, Qi, Y. Q., additional, Qian, W. B., additional, Qian, Y., additional, Qiao, C. F., additional, Qin, J. J., additional, Qin, L. Q., additional, Qin, X. S., additional, Qiu, T. L., additional, Rademacker, J., additional, Redmer, C. F., additional, Sang, H. Y., additional, Saur, M., additional, Shan, W., additional, Shan, X. Y., additional, Shang, L. L., additional, Shao, M., additional, Shekhtman, L., additional, Shen, C. P., additional, Shen, J. M., additional, Shen, Z. T., additional, Shi, H. C., additional, Shi, X. D., additional, Shwartz, B., additional, Sokolov, A., additional, Song, J. J., additional, Song, W. M., additional, Song, Y., additional, Song, Y. X., additional, Sukharev, A., additional, Sun, J. F., additional, Sun, L., additional, Sun, X. M., additional, Sun, Y. J., additional, Sun, Z. P., additional, Tang, J., additional, Tang, S. S., additional, Tang, Z. B., additional, Tian, C. H., additional, Tian, J. S., additional, Tian, Y., additional, Tikhonov, Y., additional, Todyshev, K., additional, Uglov, T., additional, Vorobyev, V., additional, Wan, B. D., additional, Wang, B. L., additional, Wang, B., additional, Wang, D. Y., additional, Wang, G. Y., additional, Wang, G. L., additional, Wang, H. L., additional, Wang, J., additional, Wang, J. H., additional, Wang, J. C., additional, Wang, M. L., additional, Wang, R., additional, Wang, S. B., additional, Wang, W., additional, Wang, W. P., additional, Wang, X. C., additional, Wang, X. D., additional, Wang, X. L., additional, Wang, X. P., additional, Wang, X. F., additional, Wang, Y. D., additional, Wang, Y. P., additional, Wang, Y. Q., additional, Wang, Y. L., additional, Wang, Y. G., additional, Wang, Z. Y., additional, Wang, Z. L., additional, Wang, Z. G., additional, Wei, D. H., additional, Wei, X. L., additional, Wei, X. M., additional, Wen, Q. G., additional, Wen, X. J., additional, Wilkinson, G., additional, Wu, B., additional, Wu, J. J., additional, Wu, L., additional, Wu, P., additional, Wu, T. W., additional, Wu, Y. S., additional, Xia, L., additional, Xiang, T., additional, Xiao, C. W., additional, Xiao, D., additional, Xiao, M., additional, Xie, K. P., additional, Xie, Y. H., additional, Xing, Y., additional, Xing, Z. Z., additional, Xiong, X. N., additional, Xu, F. R., additional, Xu, J., additional, Xu, L. L., additional, Xu, Q. N., additional, Xu, X. C., additional, Xu, X. P., additional, Xu, Y. C., additional, Xu, Y. P., additional, Xu, Y., additional, Xu, Z. Z., additional, Xuan, D. W., additional, Xue, F. F., additional, Yan, L., additional, Yan, M. J., additional, Yan, W. B., additional, Yan, W. C., additional, Yan, X. S., additional, Yang, B. F., additional, Yang, C., additional, Yang, H. J., additional, Yang, H. R., additional, Yang, H. T., additional, Yang, J. F., additional, Yang, S. L., additional, Yang, Y. D., additional, Yang, Y. H., additional, Yang, Y. S., additional, Yang, Y. L., additional, Yang, Z. W., additional, Yang, Z. Y., additional, Yao, D. L., additional, Yin, H., additional, Yin, X. H., additional, Yokozaki, N., additional, You, S. Y., additional, You, Z. Y., additional, Yu, C. X., additional, Yu, F. S., additional, Yu, G. L., additional, Yu, H. L., additional, Yu, J. S., additional, Yu, J. Q., additional, Yuan, L., additional, Yuan, X. B., additional, Yuan, Z. Y., additional, Yue, Y. F., additional, Zeng, M., additional, Zeng, S., additional, Zhang, A. L., additional, Zhang, B. W., additional, Zhang, G. Y., additional, Zhang, G. Q., additional, Zhang, H. J., additional, Zhang, H. B., additional, Zhang, J. Y., additional, Zhang, J. L., additional, Zhang, J., additional, Zhang, L., additional, Zhang, L. M., additional, Zhang, Q. A., additional, Zhang, R., additional, Zhang, S. L., additional, Zhang, T., additional, Zhang, X., additional, Zhang, Y., additional, Zhang, Y. J., additional, Zhang, Y. X., additional, Zhang, Y. T., additional, Zhang, Y. F., additional, Zhang, Y. C., additional, Zhang, Y. M., additional, Zhang, Y. L., additional, Zhang, Z. H., additional, Zhang, Z. Y., additional, Zhao, H. Y., additional, Zhao, J., additional, Zhao, L., additional, Zhao, M. G., additional, Zhao, Q., additional, Zhao, R. G., additional, Zhao, R. P., additional, Zhao, Y. X., additional, Zhao, Z. G., additional, Zhao, Z. X., additional, Zhemchugov, A., additional, Zheng, B., additional, Zheng, L., additional, Zheng, Q. B., additional, Zheng, R., additional, Zheng, Y. H., additional, Zhong, X. H., additional, Zhou, H. J., additional, Zhou, H. Q., additional, Zhou, H., additional, Zhou, S. H., additional, Zhou, X., additional, Zhou, X. K., additional, Zhou, X. P., additional, Zhou, X. R., additional, Zhou, Y. L., additional, Zhou, Y., additional, Zhou, Y. X., additional, Zhou, Z. Y., additional, Zhu, J. Y., additional, Zhu, K., additional, Zhu, R. D., additional, Zhu, R. L., additional, Zhu, S. H., additional, Zhu, Y. C., additional, Zhu, Z. A., additional, Zhukova, V., additional, Zhulanov, V., additional, Zou, B. S., additional, and Zuo, Y. B., additional
Published: 2023
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30. Symmetrically +/-45° Dual-Polarized Rectenna Array for Orthogonally and/or Two-Tone Excited Polarization-Insensitive and Wide-Coverage MPT

Author: Zhou, W. L., primary, Zhu, G. X., additional, Wang, J. C., additional, and Zhang, H., additional
Published: 2023
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31. Study on Parameters Optimisation of Fracturing Stages & Perforation Clusters in Luzhou Deep Shale Gas Horizontal Wells Based on Integrated Drilling and Logging Data

Author: Yuan, L., additional, Hu, S. L., additional, Mu, L. Y., additional, Wang, D. L., additional, Yang, X. T., additional, Song, Y., additional, and Wang, J. C., additional
Published: 2023
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32. Measurement of the Tb159(n,γ) cross section at the CSNS Back-n facility

Author: Zhang, S., primary, Li, G., additional, Jiang, W., additional, Wang, D. X., additional, Ren, J., additional, Huang, M., additional, Li, E. T., additional, Tang, J. Y., additional, Ruan, X. C., additional, Wang, H. W., additional, Li, Z. H., additional, Chen, Y. S., additional, Liu, L. X., additional, Li, X. X., additional, Fan, Q. W., additional, Fan, R. R., additional, Hu, X. R., additional, Wang, J. C., additional, Li, X., additional, Niu, D. D., additional, Song, N., additional, and Gu, M., additional
Published: 2023
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33. MICROSCALE HEAT TRANSFER AT FAST TIME STUDIED BY NOVEL LASER-BASED MEASUREMENT TECHIQUES

Author: He, K. X., primary, Wang, J. C., additional, Chow, Alan, additional, Mo, Jiada, additional, and Holden, Carl, additional
Published: 2023
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34. THE HEAT TRANSFER CHARACTERISTICS OF PHASE CHANGE HEAT STORAGE MEDIUM USED IN A HEAT PIPE TYPE SOLAR COLLECTOR

Author: Xinlin, Xia, primary, Wang, J. C. Y., additional, Jifu, Liu, additional, and Heping, Tan, additional
Published: 2023
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35. Radiation tolerance of diamond detectors

Author: Bäni, L, Artuso, M, Bachmair, F, Bartosik, M, Beck, H, Bellini, V, Belyaev, V, Bentele, B, Bergonzo, P, Bes, A, Brom, J-M, Chiodini, G, Chren, D, Cindro, V, Claus, G, Collot, J, Cumalat, J, Curtoni, S, Dabrowski, A, D'Alessandro, R, Dauvergne, D, de Boer, W, Dorfer, C, Dünser, M, Eigen, G, Eremin, V, Forneris, J, Gallin-Martel, L, Gallin-Martel, M-L, Gan, K K, Gastal, M, Ghimouz, A, Goffe, M, Goldstein, J, Golubev, A, Gorišek, A, Grigoriev, E, Grosse-Knetter, J, Grummer, A, Hiti, B, Hits, D, Hoeferkamp, M, Hofmann, T, Hosselet, J, Hügging, F, Hutson, C, Jackman, R, Janssen, J, Jennings-Moors, R, Kagan, H, Kanxheri, K, Kis, M, Kramberger, G, Kuleshov, S, Lacoste, A, Lagomarsino, S, Lo Giudice, A, Paz, I López, Lukosi, E, Maazouzi, C, Mandić, I, Marcatili, S, Marino, A, Mathieu, C, Menichelli, M, Mikuž, M, Morozzi, A, Moscatelli, F, Moss, J, Mountain, R, Oh, A, Olivero, P, Pakpour-Tabrizi, A, Passeri, D, Pernegger, H, Perrino, R, Picollo, F, Pomorski, M, Porter, A, Potenza, R, Quadt, A, Rarbi, F, Re, A, Reichmann, M, Roe, S, Rossetto, O, Becerra, D A Sanz, Schmidt, C, Schnetzer, S, Sciortino, S, Scorzoni, A, Seidel, S, Servoli, L, Smith, D S, Sopko, B, Sopko, V, Spagnolo, S, Spanier, S, Stenson, K, Stone, R, Stugu, B, Sutera, C, Traeger, M, Trischuk, W, Truccato, M, Tuvê, C, Velthuis, J, Wagner, S, Wallny, R, Wang, J C, Welch, J, Wermes, N, Wickramasinghe, J, Yamouni, M, Zalieckas, J, Zavrtanik, M, Departement Physik [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Syracuse University, CERN [Genève], Georg-August-University = Georg-August-Universität Göttingen, Istituto Nazionale di Fisica Nucleare, Sezione di Catania (INFN), Università degli studi di Catania = University of Catania (Unict), Moscow State Engineering Physics Institute (MEPhI), University of Colorado [Colorado Springs] (UCCS), University College of London [London] (UCL), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Istituto Nazionale di Fisica Nucleare, Sezione di Lecce (INFN, Sezione di Lecce), Istituto Nazionale di Fisica Nucleare (INFN), Czech Technical University in Prague (CTU), Jozef Stefan Institute [Ljubljana] (IJS), Istituto Nazionale di Fisica Nucleare [Ferrara] (INFN), Universität Karlsruhe (TH), Department of Physics [ETH Zürich] (D-PHYS), University of Bergen (UiB), A.F. Ioffe Physical-Technical Institute, Russian Academy of Sciences [Moscow] (RAS), Università degli studi di Torino = University of Turin (UNITO), Ohio State University [Columbus] (OSU), University of Bristol [Bristol], Institute of Theoretical and Experimental Physics [Moscow] (ITEP), National Research Center 'Kurchatov Institute' (NRC KI), The University of New Mexico [Albuquerque], Rheinische Friedrich-Wilhelms-Universität Bonn, Istituto Nazionale di Fisica Nucleare, Sezione di Perugia (INFN, Sezione di Perugia), GSI Helmholtzzentrum für Schwerionenforschung (GSI), Istituto Nazionale di Fisica Nucleare, Sezione di Firenze (INFN, Sezione di Firenze), University of Manchester [Manchester], The University of Tennessee [Knoxville], University of Colorado [Boulder], California State University [Sacramento], Laboratoire Capteurs Diamant (LCD-LIST), Département Métrologie Instrumentation & Information (DM2I), Laboratoire d'Intégration des Systèmes et des Technologies (LIST (CEA)), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Laboratoire d'Intégration des Systèmes et des Technologies (LIST (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Rutgers University [Camden], Rutgers University System (Rutgers), University of Toronto, RD42 Collaboration, and European Project: 654168,H2020,H2020-INFRAIA-2014-2015,AIDA-2020(2015)
Subjects: instrumentation, History, chemical vapour deposition (CVD), detector, protons, irradiation, neutrons, radiation tolerance, electrode, polycrystalline, Computer Science Applications, Education, radiation, diamond, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Detectors and Experimental Techniques, pions, ionizing radiation, nuclear instrumentation
Abstract: International audience; Diamond is used as detector material in high energy physics experiments due to its inherent radiation tolerance. The RD42 collaboration has measured the radiation tolerance of chemical vapour deposition (CVD) diamond against proton, pion, and neutron irradiation. Results of this study are summarized in this article. The radiation tolerance of diamond detectors can be further enhanced by using a 3D electrode geometry. We present preliminary results of a poly-crystalline CVD (pCVD) diamond detector with a 3D electrode geometry after irradiation and compare to planar devices of roughly the same thickness.
Published: 2022
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36. Monte Carlo Simulations on Possible Collimation Effects of Outflows to Fan Beam Emission of Ultraluminous Accreting X-Ray Pulsars

Author: Hou, X., primary, You, Y., additional, Ji, L., additional, Soria, R., additional, Zhang, S. N., additional, Ge, M. Y., additional, Tao, L., additional, Zhang, S., additional, Feng, H., additional, Zhou, M., additional, Tuo, Y. L., additional, Song, L. M., additional, and Wang, J. C., additional
Published: 2022
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37. Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud

Author: Hou, X., primary, Ge, M. Y., additional, Ji, L., additional, Zhang, S. N., additional, You, Y., additional, Tao, L., additional, Zhang, S., additional, Soria, R., additional, Feng, H., additional, Zhou, M., additional, Tuo, Y. L., additional, Song, L. M., additional, and Wang, J. C., additional
Published: 2022
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38. Effect of Interlaminar Difference on Height Propagation Behavior of Hydraulic Fracture in Lucaogou Shale

Author: Zhang, X. H., additional, Zhang, S. C., additional, Zou, Y. S., additional, Li, J. M., additional, Wang, J. C., additional, Zhu, D. Y., additional, Zhou, G. J., additional, and Yang, C., additional
Published: 2022
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39. First Integration of 10-V CMOS Logic Circuit, 20-V Gate Driver, and 600-V VDMOSFET on a 4H-SiC Single Chip

Author: Tsui, B. Y., primary, Hung, C. L., additional, Tsai, T. K., additional, Tsui, Y. C., additional, Wang, T. W., additional, Wen, Y. X., additional, Shih, C. P., additional, Wang, J. C., additional, Lin, L. J., additional, Wang, C. H., additional, Chu, K. W., additional, and Chen, P. H., additional
Published: 2022
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40. Analysis of the openings of aircraft composite laminated wing beam web under shear load

Author: Zhang, X L, primary, Wang, J C, additional, Xu, Q, additional, Wang, Y Y, additional, and Li, C Y, additional
Published: 2022
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41. Design and expected performances of the large acceptance calorimeter for the HERD space mission

Author: Pacini, L., Adriani, O., Bai, Y. -L., Bao, T. -W., Berti, E., Bottai, S., Cao, W. -W., Casaus, J., Cui, X. -Z., D’Alessandro, R., Formato, V., Gao, J. -R., Li, R., Liu, X., Lorusso, L., Lyu, L. -W., Marin, J., Martinez, G., Pizzolotto, C., Qin, J. -J., Quan, Z., Shi, D. -L., Starodubtsev, O., Tang, Z. -C., Tiberio, A., Vagelli, V., Velasco, M. A., Wang, B., Wang, Hongmei, R. -J., Z. -G., Xu, M., Yang, Y., Zhang, L., Zheng, J. -K., Alemanno, F., Aloisio, R., Altomare, G., Ambrosi, G., An, Q., Antonelli, M., Azzarello, P., Bai, L., Bai, Y. L., Bao, T. W., Barbanera, M., Barbato, F. C. T., Bernardini, P., Berti, B., Bertucci, B., X. J., Bi, Bigongiari, G., Bongi, M., Bonvicini, V., Bordas, P., Bosch-Ramon, V., Brogi, P., Cadoux, F., Campana, D., Cao, W. W., Cao, Z., Catanzani, E., Cattaneo, P. W., Chang, J., Chang, Y. H., Chen, G. M., Chen, F., Cianetti, F., Comerma, A., Cortis, D., Cui, X. H., Cui, X. Z., Dai, C., Dai, Z. G., Gaetanoe, De, Mitri, De, Palma, De, Felice, Di, Giovanni, Di, Santo, Di, Venere, Di, Dong, L., Dong, J. N., Donvito, Y. W., Duranti, G., D’Urso, M., Evoli, D., Fang, C., Fariña, K., Favre, L., Feng, Y., Feng, C. Q., Feng, H., Feng, H. B., Finetti, Z. K., Formato, N., Frieden, V., Fusco, J. M., Gao, P., Gargano, J. R., Gascon-Fora, F., Gasparrini, D., Giglietto, D., Giovacchini, N., Gomez, F., Gong, S., Gou, K., Guida, Q. B., Guo, R., Guo, D. Y., Guo, J. H., Y. Q., He, H. H., Hu, H. B., Hu, J. Y., Hu, Hu, P., Huang, Y. M., Huang, G. S., Huang, J., Huang, W. H., Huang, X. T., Huang, Y. B., Ionica, Y. F., Jouvin, M., Kotenko, L., Kyratzis, A., Marra, La, Li, D., M. J., Li, Q. Y., Li, S. L., Li, Li, T., Li, X., Li, Z., Liang, Z. H., Liang, E. W., Liao, M. J., Licciulli, C. L., Lin, F., Liu, S. J., Liu, D., Liu, H. B., Liu, H., Liu, J. B., Liu, S. B., Liu, X. W., Loparco, Y. Q., Loporchio, F., Lu, S., Lyu, X., Lyu, J. G., Maestro, L. W., Mancini, E., Manera, E., Marin, R., Marrocchesi, J., Marsella, P. S., Marzullo, M., Mauricio, D., Mocchiutti, J., Morettini, G., Mori, G., Mussolin, L., Nicola, Mazziotta, Oliva, M., Orlandi, A., Osteria, D., Pacini, G., Panico, L., Pantalei, B., Papa, F. R., Papini, S., Paredes, P., Parenti, J. M., Pauluzzi, A., Pearce, M., Peng, M., Perfetto, W. X., Perrina, F., Perrotta, C., Pillera, G., Pizzolotto, R., Qiao, C., Qin, R., Quadrani, J. J., Quan, L., Rappoldi, Z., Raselli, A., Ren, G., Renno, X. X., Ribo, F., Rico, M., Rossella, J., Ryde, M., Sanmukh, F., Scotti, A., Serini, V., Shi, D., Shi, D. L., Silveri, Q. Q., Starodubtsev, L., Su, O., D. T., Su, Sukhonos, M., Suma, D., Sun, A., Sun, X. L., Surdo, Z. T., Tang, A., Tiberio, Z. C., Tykhonov, A., Vagelli, A., Vannuccini, V., Velasco, E., Walter, M., Wang, R., Wang, A. Q., Wang, J. C., Wang, J. M., Wang, J. J., Wang, L., Wang, M., Wang, R. J., Wang, S., Wang, X. Y., Wang, X. L., Wei, Z. G., Wei, D. M., J. J., Wu, B. B., Wu, Wu, J., L. B., Wu, Wu, X., Xin, X. F., Y. L., Xu, Yan, Z. Z., Yang, H. R., Yin, Y., P. F., Yu, Yuan, Y. W., Zampa, Q., Zampa, G., Zha, N., Zhang, M., Zhang, C., Zhang, F. Z., Zhang, L. F., Zhang, S. N., Zhang, Y., Zhao, Y. L., Zheng, Z. G., Zhou, J. K., Zhu, Y. L., Zhu, F. R., and K. J.
Subjects: Space experiments, Energy, Scintillating fiber, Performance, Monte Carlo methods, Measurements of, Space stations, Space missions, Cosmology, Cosmic rays, Intelligent systems, Scintillation counters, Silicon detectors, Charge detectors, Fiber trackers, Radiation detection, Read out systems, Calorimeters
Published: 2022

42. Gamma-ray performance study of the HERD payload

Author: Adriani, O., Alemanno, F., Aloisio, R., Altomare, C., Ambrosi, G., An, Q., Antonelli, M., Azzarello, P., Bai, L., Bai, Y. L., Bao, T. W., Barbanera, M., Barbato, F. C. T., Bernardini, P., Berti, E., Bertucci, B., X. J., Bi, Bigongiari, G., Bongi, M., Bonvicini, V., Bordas, P., Bosch-Ramon, V., Bottai, S., Brogi, P., Cadoux, F., Campana, D., Cao, W. W., Cao, Z., Casaus, J., Catanzani, E., Cattaneo, P. W., Chang, J., Chang, Y. H., Chen, G. M., Chen, Y., Cianetti, F., Comerma, A., Cortis, D., Cui, X. H., Cui, X. Z., Dai, C., Dai, Z. G., D'Alessandro, R., Gaetano, De, Mitri, De, Palma, De, Felice, Di, Giovanni, Di, Santo, Di, Venere, Di, Dong, L., Dong, J. N., Donvito, Y. W., Duranti, G., D'Urso, M., Evoli, D., Fang, C., Fariña, K., Favre, L., Feng, Y., Feng, C. Q., Feng, H., Feng, H. B., Finetti, Z. K., Formato, N., Frieden, V., Fusco, J. M., Gao, P., Gargano, J. R., Gascon-Fora, F., Gasparrini, D., Giglietto, D., Giovacchini, N., Gomez, F., Gong, S., Gou, K., Guida, Q. B., Guo, R., Guo, D. Y., Guo, J. H., Y. Q., He, H. H., Hu, H. B., Hu, J. Y., Hu, Hu, P., Huang, Y. M., Huang, G. S., Huang, J., Huang, W. H., Huang, X. T., Huang, Y. B., Ionica, Y. F., Jouvin, M., Kotenko, L., Kyratzis, A., Marra, La, Li, D., M. J., Li, Q. Y., Li, Li, R., S. L., Li, Li, T., Li, X., Li, Z., Liang, Z. H., Liang, E. W., Liao, M. J., Licciulli, C. L., Lin, F., Liu, S. J., Liu, D., Liu, H. B., Liu, H., Liu, J. B., Liu, S. B., Liu, X., Liu, X. W., Loparco, Y. Q., Loporchio, F., Lu, S., Lyu, X., Lyu, J. G., Maestro, L. W., Mancini, E., Manera, E., Marin, R., Marrocchesi, J., Marsella, P. S., Martinez, G., Marzullo, M., Mauricio, D., Mocchiutti, J., Morettini, G., Mori, G., Mussolin, L., Nicola, Mazziotta, Oliva, M., Orlandi, A., Osteria, D., Pacini, G., Panico, L., Pantaleo, B., Papa, F. R., Papini, S., Paredes, P., Parenti, J. M., Pauluzzi, A., Pearce, M., Peng, M., Perfetto, W. X., Perrina, F., Perrotta, C., Pillera, G., Pizzolotto, R., Qiao, C., Qin, R., Quadrani, J. J., Quan, L., Rappoldi, Z., Raselli, A., Ren, G., Renno, X. X., Ribo, F., Rico, M., Rossella, J., Ryde, M., Sanmukh, F., Scotti, A., Serini, V., Shi, D., Shi, D. L., Silveri, Q. Q., Starodubtsev, L., Su, O., D. T., Su, Sukhonos, M., Suma, D., Sun, A., Sun, X. L., Surdo, Z. T., Tang, A., Tiberio, Z. C., Tykhonov, A., Vagelli, A., Vannuccini, V., Velasco, E., Walter, M., Wang, R., Wang, A. Q., Wang, B., Wang, J. C., Wang, J. M., Wang, J. J., Wang, L., Wang, M., Wang, R. J., Wang, S., Wang, X. Y., Wang, X. L., Wei, Z. G., Wei, D. M., J. J., Wu, B. B., Wu, Wu, J., L. B., Wu, Wu, X., Xin, X. F., Y. L., Xu, Xu, M., Yan, Z. Z., Yang, H. R., Yin, Y., P. F., Yu, Yuan, Y. W., Zampa, Q., Zampa, G., Zha, N., Zhang, M., Zhang, C., Zhang, F. Z., Zhang, L., Zhang, L. F., Zhang, S. N., Zhang, Y., Zhao, Y. L., Zheng, Z. G., Zhou, J. K., Zhu, Y. L., Zhu, F. R., and K. J.
Subjects: Energy, Performance, Cosmology, Gamma rays, Optical transfer function, Space stations, Dark matter searches, Detector geometry, Full simulations, Gamma-rays, Knee energy, Performance study, Radiation detection, Space astronomy, Cosmic rays
Published: 2022

43. The High Energy cosmic-Radiation Detector (HERD) Trigger System

Author: Velasco, M. A., Bao, T., Berti, E., Bonvicini, V., Casaus, J., Giovacchini, F., Liu, X., Marco, R., Marín, J., Martínez, G., Mori, N., Oliva, A., Pacini, L., Quan, Z., Tang, Z., Xu, M., Zampa, G., Zampa, N., Adriani, O., Alemanno, F., Aloisio, R., Altomare, G., Ambrosi, G., An, Q., Antonelli, M., Azzarello, P., Bai, L., Bai, Y. L., Bao, T. W., Barbanera, M., Barbato, F. C. T., Bernardini, B., Bertucci, B., X. J., Bi, Bigongiari, G., Bongi, M., Bordas, P., Bosch-Ramon, V., Bottai, S., Brogi, P., Cadoux, F., Campana, D., Cao, W. W., Cao, Z., Catanzani, E., Cattaneo, P. W., Chang, J., Chang, Y. H., Chen, G. M., Chen, F., Cianetti, F., Comerma, A., Cortis, D., Cui, X. H., Cui, X. Z., Dai, C., Dai, Z. G., D'Alessandro, R., Gaetanoe, De, Mitri, De, Palma, De, Felice, Di, Giovanni, Di, Santo, Di, Venere, Di, Dong, L., Dong, J. N., Donvito, Y. W., Duranti, G., D'Urso, M., Evoli, D., Fang, C., Fariña, K., Favre, L., Feng, Y., Feng, C. Q., Feng, H., Feng, H. B., Finetti, Z. K., Formato, N., Frieden, V., Fusco, J. M., Gao, P., Gargano, J. R., Gascon-Fora, F., Gasparrini, D., Giglietto, D., Gomez, N., Gong, S., Gou, K., Guida, Q. B., Guo, R., Guo, D. Y., Guo, J. H., Y. Q., He, H. H., Hu, H. B., Hu, J. Y., Hu, Hu, P., Huang, Y. M., Huang, G. S., Huang, J., Huang, W. H., Huang, X. T., Huang, Y. B., Ionica, Y. F., Jouvin, M., Kotenko, L., Kyratzis, A., Marra, La, Li, D., M. J., Li, Q. Y., Li, Li, R., S. L., Li, Li, T., Li, X., Li, Z., Liang, Z. H., Liang, E. W., Liao, M. J., Licciulli, C. L., Lin, F., Liu, S. J., Liu, D., Liu, H. B., Liu, H., Liu, J. B., Liu, S. B., Liu, X. W., Loparco, Y. Q., Loporchio, F., Lu, S., Lyu, X., Lyu, J. G., Maestro, L. W., Mancini, E., Manera, E., Marrocchesi, R., Marsella, P. S., Martinez, G., Marzullo, M., Mauricio, D., Mocchiutti, J., Morettini, G., Mussolin, L., Nicola, Mazziotta, Orlandi, M., Osteria, D., Panico, G., Pantalei, B., Papa, F. R., Papini, S., Paredes, P., Parenti, J. M., Pauluzzi, A., Pearce, M., Peng, M., Perfetto, W. X., Perrina, F., Perrotta, C., Pillera, G., Pizzolotto, R., Qiao, C., Qin, R., Quadrani, J. J., Rappoldi, L., Raselli, A., Ren, G., Renno, X. X., Ribo, F., Rico, M., Rossella, J., Ryde, M., Sanmukh, F., Scotti, A., Serini, V., Shi, D., Shi, D. L., Silveri, Q. Q., Starodubtsev, L., Su, O., D. T., Su, Sukhonos, M., Suma, D., Sun, A., Sun, X. L., Surdo, Z. T., Tang, A., Tiberio, Z. C., Tykhonov, A., Vagelli, A., Vannuccini, V., Velasco, E., Walter, M., Wang, R., Wang, A. Q., Wang, B., Wang, J. C., Wang, J. M., Wang, J. J., Wang, L., Wang, M., Wang, R. J., Wang, S., Wang, X. Y., Wang, X. L., Wei, Z. G., Wei, D. M., J. J., Wu, B. B., Wu, Wu, J., L. B., Wu, Wu, X., Xin, X. F., Y. L., Xu, Yan, Z. Z., Yang, H. R., Yin, Y., P. F., Yu, Yuan, Y. W., Zha, Q., Zhang, M., Zhang, C., Zhang, F. Z., Zhang, L., Zhang, L. F., Zhang, S. N., Zhang, Y., Zhao, Y. L., Zheng, Z. G., Zhou, J. K., Zhu, Y. L., Zhu, F. R., and K. J.
Subjects: Cosmology, Gamma rays, Intelligent systems, Monte Carlo methods, Space stations, Tellurium compounds, Topology, Dark matter, Electron spectrum, Energy, Fundamental physics, Measurements of, Plastic scintillator detector, Precise measurements, Radiation detection, Space-borne, Trigger systems, Cosmic rays
Published: 2022

44. The Plastic Scintillator Detector of the HERD space mission

Author: Kyratzis, D., Alemanno, F., Altomare, C., Barbato, F. C. T., Bernardini, P., Cattaneo, P. W., Mitri, De, Palma, De, Venere, Di, Santo, Di, Fusco, M., Gargano, P., Loparco, F., Loporchio, F., Marsella, S., Mazziotta, G., Pantaleo, M. N., Parenti, F. R., Pillera, A., Rappoldi, R., Raselli, A., Rossella, G., Serini, M., Silveri, D., Surdo, L., Wu, A., Adriani, L., Aloisio, O., Ambrosi, G., An, G., Antonelli, Q., Azzarello, M., Bai, P., Bai, L., Bao, Y. L., Barbanera, T. W., Berti, M., Bertucci, B., Bi, B., Bigongiari, X. J., Bongi, G., Bonvicini, M., Bordas, V., Bosch-Ramon, P., Bottai, V., Brogi, S., Cadoux, P., Campana, F., Cao, D., Cao, W. W., Casaus, Z., Catanzani, J., Chang, E., Chang, J., Chen, Y. H., Chen, G. M., Cianetti, F., Comerma, F., Cortis, A., Cui, D., Cui, X. H., Dai, X. Z., Dai, C., D'Alessandro, Z. G., Gaetano, De, Felice, Di, Giovanni, Di, Dong, A., Dong, J. N., Donvito, Y. W., Duranti, G., D'Urso, M., Evoli, D., Fang, C., Fariña, K., Favre, L., Feng, Y., Feng, C. Q., Feng, H., Feng, H. B., Finetti, Z. K., Formato, N., Frieden, V., Gao, J. M., Gascon-Fora, J. R., Gasparrini, D., Giglietto, D., Giovacchini, N., Gomez, F., Gong, S., Gou, K., Guida, Q. B., Guo, R., Guo, D. Y., Guo, J. H., Y. Q., He, H. H., Hu, H. B., Hu, J. Y., Hu, Hu, P., Huang, Y. M., Huang, G. S., Huang, J., Huang, W. H., Huang, X. T., Huang, Y. B., Ionica, Y. F., Jouvin, M., Kotenko, L., Marra, La, Li, D., M. J., Li, Q. Y., Li, Li, R., S. L., Li, Li, T., Li, X., Li, Z., Liang, Z. H., Liang, E. W., Liao, M. J., Licciulli, C. L., Lin, F., Liu, S. J., Liu, D., Liu, H. B., Liu, H., Liu, J. B., Liu, S. B., Liu, X., Liu, X. W., Y. Q., Lu, Lyu, X., Lyu, J. G., Maestro, L. W., Mancini, E., Manera, E., Marin, R., Marrocchesi, J., Martinez, P. S., Martinez, G., Marzullo, M., Mauricio, D., Mocchiutti, J., Morettini, G., Mori, G., Mussolin, L., Oliva, L., Orlandi, A., Osteria, D., Pacini, G., Panico, L., Papa, B., Papini, S., Paredes, P., Pauluzzi, J. M., Pearce, M., Peng, M., Perfetto, W. X., Perrina, F., Perrotta, C., Pizzolotto, G., Qiao, C., Qin, R., Quadrani, J. J., Quan, L., Ren, Z., Renno, X. X., Ribo, F., Rico, M., Ryde, J., Sanmukh, F., Scotti, A., Shi, V., Shi, D. L., Starodubtsev, Q. Q., Su, O., D. T., Su, Sukhonos, M., Suma, D., Sun, A., Sun, X. L., Tang, Z. T., Tiberio, Z. C., Tykhonov, A., Vagelli, A., Vannuccini, V., Velasco, E., Walter, M., Wang, R., Wang, A. Q., Wang, B., Wang, J. C., Wang, J. M., Wang, J. J., Wang, L., Wang, M., Wang, R. J., Wang, S., Wang, X. Y., Wang, X. L., Wei, Z. G., Wei, D. M., J. J., Wu, B. B., Wu, Wu, J., L. B., Wu, Wu, X., Xin, X. F., Y. L., Xu, Xu, M., Yan, Z. Z., Yang, H. R., Yin, Y., P. F., Yu, Yuan, Y. W., Zampa, Q., Zampa, G., Zha, N., Zhang, M., Zhang, C., Zhang, F. Z., Zhang, L., Zhang, L. F., Zhang, S. N., Zhang, Y., Zhao, Y. L., Zheng, Z. G., Zhou, J. K., Zhu, Y. L., Zhu, F. R., and K. J.
Subjects: Energy, Gamma-ray astronomy, Charged particles, Gamma rays, High energy gamma rays, Measurements of, Space-borne instruments, Space stations, Mass composition, Space missions, Cosmology, Cosmic ray energy spectrum, Plastic scintillator detector, Precise measurements, Scintillation counters, Cosmic rays
Published: 2022

45. Minimum Joint Depth for Moment Frames with HighStrength Materials.

Author: Lee, H.-J., Lequesne, R. D., Lepage, A., Lin, J.-X., Wang, J.-C., and Yin, S. Y.-L.
Subjects: CONCRETE columns, BEAM-column joints, CONCRETE
Abstract: This paper reports results from four large-scale interior beam column connections without transverse beams or slabs tested under reversed cyclic displacements. The specimens, which included the first of interior beam-column connections constructed with Grade 100 (690) reinforcement with bar deformations similar to those available in U.S. practice, had Grade 60 or 100 (420 or 690) bars, 4 or 10 ksi (28 or 69 MPa) concrete, and varied column depth to-beam bar diameter ratios. The specimens all exhibited strengths greater than the nominal strength, retained at least 80% of their strength to drift ratios exceeding 5%, and exceeded ACI 374 acceptance criteria at a 3% drift ratio for components of special moment frames, demonstrating that well-detailed joints constructed with high-strength materials behave satisfactorily. The data add evidence that joints constructed with high-strength concrete exhibit less bond decay, and recommendations are made for accounting for this effect in design. Results from the specimen constructed with normal-strength materials, considered in the context of prior tests, suggest a need to increase the minimum joint depth for special moment frames. Considerable improvement in behavior associated with reduced bond damage within the joint is obtained from a 20% increase in the minimum column depth-to-beam bar diameter ratio required in ACI 318-19. [ABSTRACT FROM AUTHOR]
Published: 2023
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46. [Artificial intelligence model for diagnosis of coronary artery disease based on facial photos].

Author: Lin L, Xu TF, Ding YD, Zhang Y, Wang JC, Zuo YX, Zhang G, Wang MX, and Zeng Y
Subjects: Humans, Cross-Sectional Studies, Coronary Angiography methods, Photography methods, Male, Coronary Artery Disease diagnosis, Coronary Artery Disease diagnostic imaging, Artificial Intelligence, Face diagnostic imaging
Abstract: Objective: To develop and validate an artificial intelligence (AI) diagnostic model for coronary artery disease based on facial photos. Methods: This study was a cross-sectional study. Patients who were scheduled to undergo coronary angiography (CAG) at Beijing Anzhen Hospital and Beijing Daxing Hospital from August 2022 to November 2023 were included consecutively. Before CAG, facial photos were collected (including four angles: frontal view, left and right 60° profile, and top of the head). Photo datasets were randomly divided into a training set, a validation set (70%), and a testing set (30%). The model was constructed using Masked Autoencoder (MAE) and Vision Transformer (ViT) architectures. Firstly, the model base was pre-training using 2 million facial photos obtained from the publicly available VGGFace dataset, and fine-tuned by the training and validation sets; the model was validated in the test set. In addition, the ResNet architecture was used to process the dataset, and its outputs were compared with those of the models based on MAE and ViT. In the test set, the area under the operating characteristic curve ( AUC ) of the AI model was calculated using CAG results as the gold standard. Results: A total of 5 974 participants aged 61 (54, 67) years were included, including 4 179 males (70.0%), with a total of 84 964 facial photos. There were 79 140 facial photos in the training and validation sets, with 3 822 patients with coronary artery disease; there were 5 824 facial photos in the test set, with 239 patients with coronary artery disease. The AUC value of the MAE and ViT model initialized with pre-training model weights was 0.841 and 0.824, respectively. The AUC of the ResNet model initialized with random weights was 0.810, while the AUC of the ResNet model initialized with pre-training model weights was 0.816. Conclusion: The AI model based on facial photos showes good diagnostic performance for coronary artery disease and holds promise for further application in early diagnosis.
Published: 2024
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47. [4 cases of occupational lung cancer caused by chloromethyl ether and dichloromethyl ether in a chemical enterprise].

Author: Song LK, Wang JC, Tian QJ, and Zhang P
Subjects: Humans, Male, Middle Aged, Adult, Chemical Industry, Lung Neoplasms chemically induced, Occupational Exposure adverse effects, Occupational Diseases chemically induced
Abstract: Chloromethyl ether and diclomethyl ether are statutory substances that cause occupational lung cancer. From 2021 to 2022, the Department of Occupational Diseases of the Eighth People's Hospital of Hebei Province successively received 4 cases of lung cancer from a chemical company that required occupational disease diagnosis. All four patients had a clear occupational history of chloromethyl ether and diclomethyl ether for more than 1 year, diagnosis of primary small cell lung cancer supported by relevant histopathology, immunohistochemistry, and tumor markers. All the 4 patients were diagnosed as occupational lung cancer (chloromethyl ether, diclomethyl ether) .
Published: 2024
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48. Stringent Tests of Lorentz Invariance Violation from LHAASO Observations of GRB 221009A.

Author: Cao Z, Aharonian F, Axikegu, Bai YX, Bao YW, Bastieri D, Bi XJ, Bi YJ, Bian W, Bukevich AV, Cao Q, Cao WY, Cao Z, Chang J, Chang JF, Chen AM, Chen ES, Chen HX, Chen L, Chen L, Chen L, Chen MJ, Chen ML, Chen QH, Chen S, Chen SH, Chen SZ, Chen TL, Chen Y, Cheng N, Cheng YD, Cui MY, Cui SW, Cui XH, Cui YD, Dai BZ, Dai HL, Dai ZG, Danzengluobu, Dong XQ, Duan KK, Fan JH, Fan YZ, Fang J, Fang JH, Fang K, Feng CF, Feng H, Feng L, Feng SH, Feng XT, Feng Y, Feng YL, Gabici S, Gao B, Gao CD, Gao Q, Gao W, Gao WK, Ge MM, Geng LS, Giacinti G, Gong GH, Gou QB, Gu MH, Guo FL, Guo XL, Guo YQ, Guo YY, Han YA, Hasan M, He HH, He HN, He JY, He Y, Hor YK, Hou BW, Hou C, Hou X, Hu HB, Hu Q, Hu SC, Huang DH, Huang TQ, Huang WJ, Huang XT, Huang XY, Huang Y, Ji XL, Jia HY, Jia K, Jiang K, Jiang XW, Jiang ZJ, Jin M, Kang MM, Karpikov I, Kuleshov D, Kurinov K, Li BB, Li CM, Li C, Li C, Li D, Li F, Li HB, Li HC, Li J, Li J, Li K, Li SD, Li WL, Li WL, Li XR, Li X, Li YZ, Li Z, Li Z, Liang EW, Liang YF, Lin SJ, Liu B, Liu C, Liu D, Liu DB, Liu H, Liu HD, Liu J, Liu JL, Liu MY, Liu RY, Liu SM, Liu W, Liu Y, Liu YN, Luo Q, Luo Y, Lv HK, Ma BQ, Ma LL, Ma XH, Mao JR, Min Z, Mitthumsiri W, Mu HJ, Nan YC, Neronov A, Ou LJ, Pattarakijwanich P, Pei ZY, Qi JC, Qi MY, Qiao BQ, Qin JJ, Raza A, Ruffolo D, Sáiz A, Saeed M, Semikoz D, Shao L, Shchegolev O, Sheng XD, Shu FW, Song HC, Stenkin YV, Stepanov V, Su Y, Sun DX, Sun QN, Sun XN, Sun ZB, Takata J, Tam PHT, Tang QW, Tang R, Tang ZB, Tian WW, Wang C, Wang CB, Wang GW, Wang HG, Wang HH, Wang JC, Wang K, Wang K, Wang LP, Wang LY, Wang PH, Wang R, Wang W, Wang XG, Wang XY, Wang Y, Wang YD, Wang YJ, Wang ZH, Wang ZX, Wang Z, Wang Z, Wei DM, Wei JJ, Wei YJ, Wen T, Wu CY, Wu HR, Wu QW, Wu S, Wu XF, Wu YS, Xi SQ, Xia J, Xiang GM, Xiao DX, Xiao G, Xin YL, Xing Y, Xiong DR, Xiong Z, Xu DL, Xu RF, Xu RX, Xu WL, Xue L, Yan DH, Yan JZ, Yan T, Yang CW, Yang CY, Yang F, Yang FF, Yang LL, Yang MJ, Yang RZ, Yang WX, Yao YH, Yao ZG, Yin LQ, Yin N, You XH, You ZY, Yu YH, Yuan Q, Yue H, Zeng HD, Zeng TX, Zeng W, Zha M, Zhang BB, Zhang F, Zhang H, Zhang HM, Zhang HY, Zhang JL, Zhang L, Zhang PF, Zhang PP, Zhang R, Zhang SB, Zhang SR, Zhang SS, Zhang X, Zhang XP, Zhang YF, Zhang Y, Zhang Y, Zhao B, Zhao J, Zhao L, Zhao LZ, Zhao SP, Zhao XH, Zheng F, Zhong WJ, Zhou B, Zhou H, Zhou JN, Zhou M, Zhou P, Zhou R, Zhou XX, Zhou XX, Zhu BY, Zhu CG, Zhu FR, Zhu H, Zhu KJ, Zou YC, and Zuo X
Abstract: On 9 October 2022, the Large High Altitude Air Shower Observatory (LHAASO) reported the observation of the very early TeV afterglow of the brightest-of-all-time gamma-ray burst 221009A, recording the highest photon statistics in the TeV band ever obtained from a gamma-ray burst. We use this unique observation to place stringent constraints on the energy dependence of the speed of light in vacuum, a manifestation of Lorentz invariance violation (LIV) predicted by some quantum gravity (QG) theories. Our results show that the 95% confidence level lower limits on the QG energy scales are E_{QG,1}>10 times the Planck energy E_{Pl} for the linear LIV effect, and E_{QG,2}>6×10^{-8}E_{Pl} for the quadratic LIV effect. Our limits on the quadratic LIV case improve previous best bounds by factors of 5-7.
Published: 2024
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49. Constraints on Ultraheavy Dark Matter Properties from Dwarf Spheroidal Galaxies with LHAASO Observations.

Author: Cao Z, Aharonian F, An Q, Axikegu, Bai YX, Bao YW, Bastieri D, Bi XJ, Bi YJ, Cai JT, Cao Q, Cao WY, Cao Z, Chang J, Chang JF, Chen AM, Chen ES, Chen L, Chen L, Chen L, Chen MJ, Chen ML, Chen QH, Chen SH, Chen SZ, Chen TL, Chen Y, Cheng N, Cheng YD, Cui MY, Cui SW, Cui XH, Cui YD, Dai BZ, Dai HL, Dai ZG, Danzengluobu, Della Volpe D, Dong XQ, Duan KK, Fan JH, Fan YZ, Fang J, Fang K, Feng CF, Feng L, Feng SH, Feng XT, Feng YL, Gabici S, Gao B, Gao CD, Gao LQ, Gao Q, Gao W, Gao WK, Ge MM, Geng LS, Giacinti G, Gong GH, Gou QB, Gu MH, Guo FL, Guo XL, Guo YQ, Guo YY, Han YA, He HH, He HN, He JY, He XB, He Y, Heller M, Hor YK, Hou BW, Hou C, Hou X, Hu HB, Hu Q, Hu SC, Huang DH, Huang TQ, Huang WJ, Huang XT, Huang XY, Huang Y, Huang ZC, Ji XL, Jia HY, Jia K, Jiang K, Jiang XW, Jiang ZJ, Jin M, Kang MM, Ke T, Kuleshov D, Kurinov K, Li BB, Li C, Li C, Li D, Li F, Li HB, Li HC, Li HY, Li J, Li J, Li J, Li K, Li WL, Li WL, Li XR, Li X, Li YZ, Li Z, Li Z, Liang EW, Liang YF, Lin SJ, Liu B, Liu C, Liu D, Liu H, Liu HD, Liu J, Liu JL, Liu JY, Liu MY, Liu RY, Liu SM, Liu W, Liu Y, Liu YN, Lu R, Luo Q, Lv HK, Ma BQ, Ma LL, Ma XH, Mao JR, Min Z, Mitthumsiri W, Mu HJ, Nan YC, Neronov A, Ou ZW, Pang BY, Pattarakijwanich P, Pei ZY, Qi MY, Qi YQ, Qiao BQ, Qin JJ, Ruffolo D, Sáiz A, Semikoz D, Shao CY, Shao L, Shchegolev O, Sheng XD, Shu FW, Song HC, Stenkin YV, Stepanov V, Su Y, Sun QN, Sun XN, Sun ZB, Tam PHT, Tang QW, Tang ZB, Tian WW, Wang C, Wang CB, Wang GW, Wang HG, Wang HH, Wang JC, Wang K, Wang LP, Wang LY, Wang PH, Wang R, Wang W, Wang XG, Wang XY, Wang Y, Wang YD, Wang YJ, Wang ZH, Wang ZX, Wang Z, Wang Z, Wei DM, Wei JJ, Wei YJ, Wen T, Wu CY, Wu HR, Wu S, Wu XF, Wu YS, Xi SQ, Xia J, Xia JJ, Xiang GM, Xiao DX, Xiao G, Xin GG, Xin YL, Xing Y, Xiong Z, Xu DL, Xu RF, Xu RX, Xu WL, Xue L, Yan DH, Yan JZ, Yan T, Yang CW, Yang F, Yang FF, Yang HW, Yang JY, Yang LL, Yang MJ, Yang RZ, Yang SB, Yao YH, Yao ZG, Ye YM, Yin LQ, Yin N, You XH, You ZY, Yu YH, Yuan Q, Yue H, Zeng HD, Zeng TX, Zeng W, Zha M, Zhang BB, Zhang F, Zhang HM, Zhang HY, Zhang JL, Zhang LX, Zhang L, Zhang PF, Zhang PP, Zhang R, Zhang SB, Zhang SR, Zhang SS, Zhang X, Zhang XP, Zhang YF, Zhang Y, Zhang Y, Zhao B, Zhao J, Zhao L, Zhao LZ, Zhao SP, Zheng F, Zhou B, Zhou H, Zhou JN, Zhou M, Zhou P, Zhou R, Zhou XX, Zhu CG, Zhu FR, Zhu H, Zhu KJ, and Zuo X
Abstract: In this Letter we try to search for signals generated by ultraheavy dark matter at the Large High Altitude Air Shower Observatory (LHAASO) data. We look for possible γ rays by dark matter annihilation or decay from 16 dwarf spheroidal galaxies in the field of view of the LHAASO. Dwarf spheroidal galaxies are among the most promising targets for indirect detection of dark matter that have low fluxes of astrophysical γ-ray background while having large amount of dark matter. By analyzing more than 700 days of observational data at LHAASO, no significant dark matter signal from 1 TeV to 1 EeV is detected. Accordingly we derive the most stringent constraints on the ultraheavy dark matter annihilation cross section up to EeV. The constraints on the lifetime of dark matter in decay mode are also derived.
Published: 2024
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50. Measurements of All-Particle Energy Spectrum and Mean Logarithmic Mass of Cosmic Rays from 0.3 to 30 PeV with LHAASO-KM2A.

Author: Cao Z, Aharonian F, Axikegu, Bai YX, Bao YW, Bastieri D, Bi XJ, Bi YJ, Bian W, Bukevich AV, Cao Q, Cao WY, Cao Z, Chang J, Chang JF, Chen AM, Chen ES, Chen HX, Chen L, Chen L, Chen L, Chen MJ, Chen ML, Chen QH, Chen S, Chen SH, Chen SZ, Chen TL, Chen Y, Cheng N, Cheng YD, Cui MY, Cui SW, Cui XH, Cui YD, Dai BZ, Dai HL, Dai ZG, Danzengluobu, Dong XQ, Duan KK, Fan JH, Fan YZ, Fang J, Fang JH, Fang K, Feng CF, Feng H, Feng L, Feng SH, Feng XT, Feng Y, Feng YL, Gabici S, Gao B, Gao CD, Gao Q, Gao W, Gao WK, Ge MM, Geng LS, Giacinti G, Gong GH, Gou QB, Gu MH, Guo FL, Guo XL, Guo YQ, Guo YY, Han YA, Hasan M, He HH, He HN, He JY, He Y, Hor YK, Hou BW, Hou C, Hou X, Hu HB, Hu Q, Hu SC, Huang DH, Huang TQ, Huang WJ, Huang XT, Huang XY, Huang Y, Ji XL, Jia HY, Jia K, Jiang K, Jiang XW, Jiang ZJ, Jin M, Kang MM, Karpikov I, Kuleshov D, Kurinov K, Li BB, Li CM, Li C, Li C, Li D, Li F, Li HB, Li HC, Li J, Li J, Li K, Li SD, Li WL, Li WL, Li XR, Li X, Li YZ, Li Z, Li Z, Liang EW, Liang YF, Lin SJ, Liu B, Liu C, Liu D, Liu DB, Liu H, Liu HD, Liu J, Liu JL, Liu MY, Liu RY, Liu SM, Liu W, Liu Y, Liu YN, Luo Q, Luo Y, Lv HK, Ma BQ, Ma LL, Ma XH, Mao JR, Min Z, Mitthumsiri W, Mu HJ, Nan YC, Neronov A, Ou LJ, Pattarakijwanich P, Pei ZY, Qi JC, Qi MY, Qiao BQ, Qin JJ, Raza A, Ruffolo D, Sáiz A, Saeed M, Semikoz D, Shao L, Shchegolev O, Sheng XD, Shu FW, Song HC, Stenkin YV, Stepanov V, Su Y, Sun DX, Sun QN, Sun XN, Sun ZB, Takata J, Tam PHT, Tang QW, Tang R, Tang ZB, Tian WW, Wang C, Wang CB, Wang GW, Wang HG, Wang HH, Wang JC, Wang K, Wang K, Wang LP, Wang LY, Wang PH, Wang R, Wang W, Wang XG, Wang XY, Wang Y, Wang YD, Wang YJ, Wang ZH, Wang ZX, Wang Z, Wang Z, Wei DM, Wei JJ, Wei YJ, Wen T, Wu CY, Wu HR, Wu QW, Wu S, Wu XF, Wu YS, Xi SQ, Xia J, Xiang GM, Xiao DX, Xiao G, Xin YL, Xing Y, Xiong DR, Xiong Z, Xu DL, Xu RF, Xu RX, Xu WL, Xue L, Yan DH, Yan JZ, Yan T, Yang CW, Yang CY, Yang F, Yang FF, Yang LL, Yang MJ, Yang RZ, Yang WX, Yao YH, Yao ZG, Yin LQ, Yin N, You XH, You ZY, Yu YH, Yuan Q, Yue H, Zeng HD, Zeng TX, Zeng W, Zha M, Zhang BB, Zhang F, Zhang H, Zhang HM, Zhang HY, Zhang JL, Zhang L, Zhang PF, Zhang PP, Zhang R, Zhang SB, Zhang SR, Zhang SS, Zhang X, Zhang XP, Zhang YF, Zhang Y, Zhang Y, Zhao B, Zhao J, Zhao L, Zhao LZ, Zhao SP, Zhao XH, Zheng F, Zhong WJ, Zhou B, Zhou H, Zhou JN, Zhou M, Zhou P, Zhou R, Zhou XX, Zhou XX, Zhu BY, Zhu CG, Zhu FR, Zhu H, Zhu KJ, Zou YC, and Zuo X
Abstract: We present the measurements of all-particle energy spectrum and mean logarithmic mass of cosmic rays in the energy range of 0.3-30 PeV using data collected from LHAASO-KM2A between September 2021 and December 2022, which is based on a nearly composition-independent energy reconstruction method, achieving unprecedented accuracy. Our analysis reveals the position of the knee at 3.67±0.05±0.15 PeV. Below the knee, the spectral index is found to be -2.7413±0.0004±0.0050, while above the knee, it is -3.128±0.005±0.027, with the sharpness of the transition measured with a statistical error of 2%. The mean logarithmic mass of cosmic rays is almost heavier than helium in the whole measured energy range. It decreases from 1.7 at 0.3 PeV to 1.3 at 3 PeV, representing a 24% decline following a power law with an index of -0.1200±0.0003±0.0341. This is equivalent to an increase in abundance of light components. Above the knee, the mean logarithmic mass exhibits a power law trend towards heavier components, which is reversal to the behavior observed in the all-particle energy spectrum. Additionally, the knee position and the change in power-law index are approximately the same. These findings suggest that the knee observed in the all-particle spectrum corresponds to the knee of the light component, rather than the medium-heavy components.
Published: 2024
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