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1. Charged-current non-standard neutrino interactions at Daya Bay

Author: The Daya Bay collaboration, F. P. An, W. D. Bai, A. B. Balantekin, M. Bishai, S. Blyth, G. F. Cao, J. Cao, J. F. Chang, Y. Chang, H. S. Chen, H. Y. Chen, S. M. Chen, Y. Chen, Y. X. Chen, Z. Y. Chen, J. Cheng, Y.-C. Cheng, Z. K. Cheng, J. J. Cherwinka, M. C. Chu, J. P. Cummings, O. Dalager, F. S. Deng, X. Y. Ding, Y. Y. Ding, M. V. Diwan, T. Dohnal, D. Dolzhikov, J. Dove, K. V. Dugas, H. Y. Duyang, D. A. Dwyer, J. P. Gallo, M. Gonchar, G. H. Gong, H. Gong, W. Q. Gu, J. Y. Guo, L. Guo, X. H. Guo, Y. H. Guo, Z. Guo, R. W. Hackenburg, Y. Han, S. Hans, M. He, K. M. Heeger, Y. K. Heng, Y. K. Hor, Y. B. Hsiung, B. Z. Hu, J. R. Hu, T. Hu, Z. J. Hu, H. X. Huang, J. H. Huang, X. T. Huang, Y. B. Huang, P. Huber, D. E. Jaffe, K. L. Jen, X. L. Ji, X. P. Ji, R. A. Johnson, D. Jones, L. Kang, S. H. Kettell, S. Kohn, M. Kramer, T. J. Langford, J. Lee, J. H. C. Lee, R. T. Lei, R. Leitner, J. K. C. Leung, F. Li, H. L. Li, J. J. Li, Q. J. Li, R. H. Li, S. Li, S. C. Li, W. D. Li, X. N. Li, X. Q. Li, Y. F. Li, Z. B. Li, H. Liang, C. J. Lin, G. L. Lin, S. Lin, J. J. Ling, J. M. Link, L. Littenberg, B. R. Littlejohn, J. C. Liu, J. L. Liu, J. X. Liu, C. Lu, H. Q. Lu, K. B. Luk, B. Z. Ma, X. B. Ma, X. Y. Ma, Y. Q. Ma, R. C. Mandujano, C. Marshall, K. T. McDonald, R. D. McKeown, Y. Meng, J. Napolitano, D. Naumov, E. Naumova, T. M. T. Nguyen, J. P. Ochoa-Ricoux, A. Olshevskiy, J. Park, S. Patton, J. C. Peng, C. S. J. Pun, F. Z. Qi, M. Qi, X. Qian, N. Raper, J. Ren, C. Morales Reveco, R. Rosero, B. Roskovec, X. C. Ruan, B. Russell, H. Steiner, J. L. Sun, T. Tmej, W.-H. Tse, C. E. Tull, Y. C. Tung, B. Viren, V. Vorobel, C. H. Wang, J. Wang, M. Wang, N. Y. Wang, R. G. Wang, W. Wang, X. Wang, Y. F. Wang, Z. Wang, Z. M. Wang, H. Y. Wei, L. H. Wei, W. Wei, L. J. Wen, K. Whisnant, C. G. White, H. L. H. Wong, E. Worcester, D. R. Wu, Q. Wu, W. J. Wu, D. M. Xia, Z. Q. Xie, Z. Z. Xing, H. K. Xu, J. L. Xu, T. Xu, T. Xue, C. G. Yang, L. Yang, Y. Z. Yang, H. F. Yao, M. Ye, M. Yeh, B. L. Young, H. Z. Yu, Z. Y. Yu, B. B. Yue, V. Zavadskyi, S. Zeng, Y. Zeng, L. Zhan, C. Zhang, F. Y. Zhang, H. H. Zhang, J. L. Zhang, J. W. Zhang, Q. M. Zhang, S. Q. Zhang, X. T. Zhang, Y. M. Zhang, Y. X. Zhang, Y. Y. Zhang, Z. J. Zhang, Z. P. Zhang, Z. Y. Zhang, J. Zhao, R. Z. Zhao, L. Zhou, H. L. Zhuang, and J. H. Zou
Subjects: Neutrino Mixing, Non-Standard Neutrino Properties, Neutrino Interactions, SMEFT, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract The full data set of the Daya Bay reactor neutrino experiment is used to probe the effect of the charged current non-standard interactions (CC-NSI) on neutrino oscillation experiments. Two different approaches are applied and constraints on the corresponding CC-NSI parameters are obtained with the neutrino flux taken from the Huber-Mueller model with a 5% uncertainty. For the quantum mechanics-based approach (QM-NSI), the constraints on the CC-NSI parameters ϵ eα and ϵ eα s $$ {\epsilon}_{e\alpha}^s $$ are extracted with and without the assumption that the effects of the new physics are the same in the production and detection processes, respectively. The approach based on the weak effective field theory (WEFT-NSI) deals with four types of CC-NSI represented by the parameters [ε X ] eα . For both approaches, the results for the CC-NSI parameters are shown for cases with various fixed values of the CC-NSI and the Dirac CP-violating phases, and when they are allowed to vary freely. We find that constraints on the QM-NSI parameters ϵ eα and ϵ eα s $$ {\epsilon}_{e\alpha}^s $$ from the Daya Bay experiment alone can reach the order O $$ \mathcal{O} $$ (0.01) for the former and O $$ \mathcal{O} $$ (0.1) for the latter, while for WEFT-NSI parameters [ε X ] eα , we obtain O $$ \mathcal{O} $$ (0.1) for both cases.
Published: 2024
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2. Extraction of the ^{235}U and ^{239}Pu Antineutrino Spectra at Daya Bay

Author: D, Adey, F P, An, A B, Balantekin, H R, Band, M, Bishai, S, Blyth, D, Cao, G F, Cao, J, Cao, J F, Chang, Y, Chang, H S, Chen, S M, Chen, Y, Chen, Y X, Chen, J, Cheng, Z K, Cheng, J J, Cherwinka, M C, Chu, A, Chukanov, J P, Cummings, N, Dash, F S, Deng, Y Y, Ding, M V, Diwan, T, Dohnal, J, Dove, M, Dvořák, D A, Dwyer, M, Gonchar, G H, Gong, H, Gong, W Q, Gu, J Y, Guo, L, Guo, X H, Guo, Y H, Guo, Z, Guo, R W, Hackenburg, S, Hans, M, He, K M, Heeger, Y K, Heng, A, Higuera, Y K, Hor, Y B, Hsiung, B Z, Hu, J R, Hu, T, Hu, Z J, Hu, H X, Huang, X T, Huang, Y B, Huang, P, Huber, D E, Jaffe, K L, Jen, X L, Ji, X P, Ji, R A, Johnson, D, Jones, L, Kang, S H, Kettell, L W, Koerner, S, Kohn, M, Kramer, T J, Langford, J, Lee, J H C, Lee, R T, Lei, R, Leitner, J K C, Leung, C, Li, F, Li, H L, Li, Q J, Li, S, Li, S C, Li, S J, Li, W D, Li, X N, Li, X Q, Li, Y F, Li, Z B, Li, H, Liang, C J, Lin, G L, Lin, S, Lin, J J, Ling, J M, Link, L, Littenberg, B R, Littlejohn, J C, Liu, J L, Liu, Y, Liu, Y H, Liu, C, Lu, H Q, Lu, J S, Lu, K B, Luk, X B, Ma, X Y, Ma, Y Q, Ma, C, Marshall, D A, Martinez Caicedo, K T, McDonald, R D, McKeown, I, Mitchell, L, Mora Lepin, J, Napolitano, D, Naumov, E, Naumova, J P, Ochoa-Ricoux, A, Olshevskiy, H-R, Pan, J, Park, S, Patton, V, Pec, J C, Peng, L, Pinsky, C S J, Pun, F Z, Qi, M, Qi, X, Qian, N, Raper, J, Ren, R, Rosero, B, Roskovec, X C, Ruan, H, Steiner, J L, Sun, K, Treskov, W-H, Tse, C E, Tull, B, Viren, V, Vorobel, C H, Wang, J, Wang, M, Wang, N Y, Wang, R G, Wang, W, Wang, X, Wang, Y, Wang, Y F, Wang, Z, Wang, Z M, Wang, H Y, Wei, L H, Wei, L J, Wen, K, Whisnant, C G, White, H L H, Wong, S C F, Wong, E, Worcester, Q, Wu, W J, Wu, D M, Xia, Z Z, Xing, J L, Xu, T, Xue, C G, Yang, L, Yang, M S, Yang, Y Z, Yang, M, Ye, M, Yeh, B L, Young, H Z, Yu, Z Y, Yu, B B, Yue, S, Zeng, Y, Zeng, L, Zhan, C, Zhang, C C, Zhang, F Y, Zhang, H H, Zhang, J W, Zhang, Q M, Zhang, R, Zhang, X F, Zhang, X T, Zhang, Y M, Zhang, Y X, Zhang, Y Y, Zhang, Z J, Zhang, Z P, Zhang, Z Y, Zhang, J, Zhao, L, Zhou, H L, Zhuang, and J H, Zou
Abstract: This Letter reports the first extraction of individual antineutrino spectra from ^{235}U and ^{239}Pu fission and an improved measurement of the prompt energy spectrum of reactor antineutrinos at Daya Bay. The analysis uses 3.5×10^{6} inverse beta-decay candidates in four near antineutrino detectors in 1958 days. The individual antineutrino spectra of the two dominant isotopes, ^{235}U and ^{239}Pu, are extracted using the evolution of the prompt spectrum as a function of the isotope fission fractions. In the energy window of 4-6 MeV, a 7% (9%) excess of events is observed for the ^{235}U (^{239}Pu) spectrum compared with the normalized Huber-Mueller model prediction. The significance of discrepancy is 4.0σ for ^{235}U spectral shape compared with the Huber-Mueller model prediction. The shape of the measured inverse beta-decay prompt energy spectrum disagrees with the prediction of the Huber-Mueller model at 5.3σ. In the energy range of 4-6 MeV, a maximal local discrepancy of 6.3σ is observed.
Published: 2019

3. Publisher’s Note: Measurement of cosmic-ray muons and muon-induced neutrons in the Aberdeen Tunnel Underground Laboratory [Phys. Rev. D 93 , 072005 (2016)]

Author: H. H. C. Wong, B. Z. Hu, M. W. Kwok, Y. K. Hor, S. Y. Ngan, T. H. Ho, X. C. Chen, Y. B. Hsiung, H. L. H. Wong, M. C. Chu, K. Y. Leung, K. Shih, C. H. Wang, W. H. Luk, M. Yeh, K. B. Luk, T. Kwok, C. S. J. Pun, W. K. Ngai, K. K. Wong, G. L. Lin, Y. H. Tam, R. H. M. Tsang, K. P. Lee, R. L. Hahn, Y. P. Lau, J. K. C. Leung, C. M. Wong, K. X. Cui, K. K. Kwan, H. Y. Ngai, Y. L. Chan, Y. C. Lin, and Simon Blyth
Subjects: Physics, Nuclear physics, Muon, 010308 nuclear & particles physics, Cosmic ray muons, 0103 physical sciences, Underground laboratory, Neutron, 010306 general physics, 01 natural sciences
Published: 2016
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4. Study of $J/ψ\to p\bar{p}$ and $J/ψ\to n\bar{n}$

Author: BESIII Collaboration, M. Ablikim(Institute of High Energy Physics, Beijing, P. R. China), M. N. Achasov(G.I. Budker Institute of Nuclear Physics SB RAS), D. J. Ambrose(University of Rochester, Rochester, New York, USA), F. F. An(Institute of High Energy Physics, Beijing, P. R. China), Q. An(University of Science and Technology of China, Hefei, P. R. China), Z. H. An(Institute of High Energy Physics, Beijing, P. R. China), J. Z. Bai(Institute of High Energy Physics, Beijing, P. R. China), R. B. Ferroli(INFN Laboratori Nazionali di Frascati, Frascati, Italy), Y. Ban(Peking University, Beijing, P. R. China), J. Becker(Bochum Ruhr-University, Bochum, Germany), N. Berger(Institute of High Energy Physics, Beijing, P. R. China), M. B. Bertani(INFN Laboratori Nazionali di Frascati, Frascati, Italy), J. M. Bian(University of Minnesota, Minneapolis, MN, USA), E. Boger(20, a), O. Bondarenko(KVI/University of Groningen, Groningen, The Netherlands), I. Boyko(Joint Institute for Nuclear Research, Dubna, Russia), R. A. Briere(Carnegie Mellon University, Pittsburgh, PA, USA), V. Bytev(Joint Institute for Nuclear Research, Dubna, Russia), X. Cai(Institute of High Energy Physics, Beijing, P. R. China), A. C. Calcaterra(INFN Laboratori Nazionali di Frascati, Frascati, Italy), G. F. Cao(Institute of High Energy Physics, Beijing, P. R. China), J. F. Chang(Institute of High Energy Physics, Beijing, P. R. China), G. Chelkov(20, a), G. Chen(Institute of High Energy Physics, Beijing, P. R. China), H. S. Chen(Institute of High Energy Physics, Beijing, P. R. China), J. C. Chen(Institute of High Energy Physics, Beijing, P. R. China), M. L. Chen(Institute of High Energy Physics, Beijing, P. R. China), S. J. Chen(Nanjing University, Nanjing, P. R. China), Y. Chen(Institute of High Energy Physics, Beijing, P. R. China), Y. B. Chen(Institute of High Energy Physics, Beijing, P. R. China), H. P. Cheng(Huangshan College, Huangshan, P. R. China), Y. P. Chu(Institute of High Energy Physics, Beijing, P. R. China), D. Cronin-Hennessy(University of Minnesota, Minneapolis, MN, USA), H. L. Dai(Institute of High Energy Physics, Beijing, P. R. China), J. P. Dai(Institute of High Energy Physics, Beijing, P. R. China), D. Dedovich(Joint Institute for Nuclear Research, Dubna, Russia), Z. Y. Deng(Institute of High Energy Physics, Beijing, P. R. China), A. Denig(Johannes Gutenberg University of Mainz, Mainz, Germany), I. Denysenko(20, b), M. Destefanis(University of Turin and INFN, Turin, Italy), W. M. Ding(Shandong University, Jinan, P. R. China), Y. Ding(Liaoning University, Shenyang, P. R. China), L. Y. Dong(Institute of High Energy Physics, Beijing, P. R. China), M. Y. Dong(Institute of High Energy Physics, Beijing, P. R. China), S. X. Du(Zhengzhou University, Zhengzhou, P. R. China), J. Fang(Institute of High Energy Physics, Beijing, P. R. China), S. S. Fang(Institute of High Energy Physics, Beijing, P. R. China), L. Fava(44, c), F. Feldbauer(Bochum Ruhr-University, Bochum, Germany), C. Q. Feng(University of Science and Technology of China, Hefei, P. R. China), C. D. Fu(Institute of High Energy Physics, Beijing, P. R. China), J. L. Fu(Nanjing University, Nanjing, P. R. China), Y. Gao(Tsinghua University, Beijing, P. R. China), C. Geng(University of Science and Technology of China, Hefei, P. R. China), K. Goetzen(GSI Helmholtzcentre for Heavy Ion Research GmbH, Darmstadt, Germany), W. X. Gong(Institute of High Energy Physics, Beijing, P. R. China), W. Gradl(Johannes Gutenberg University of Mainz, Mainz, Germany), M. Greco(University of Turin and INFN, Turin, Italy), M. H. Gu(Institute of High Energy Physics, Beijing, P. R. China), Y. T. Gu(GuangXi University, Nanning, P.R.China), Y. H. Guan(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), A. Q. Guo(Nankai University, Tianjin, P. R. China), L. B. Guo(Nanjing Normal University, Nanjing, P. R. China), Y. P. Guo(Nankai University, Tianjin, P. R. China), Y. L. Han(Institute of High Energy Physics, Beijing, P. R. China), X. Q. Hao(Institute of High Energy Physics, Beijing, P. R. China), F. A. Harris(University of Hawaii, Honolulu, Hawaii, USA), K. L. He(Institute of High Energy Physics, Beijing, P. R. China), M. He(Institute of High Energy Physics, Beijing, P. R. China), Z. Y. He(Nankai University, Tianjin, P. R. China), T. Held(Bochum Ruhr-University, Bochum, Germany), Y. K. Heng(Institute of High Energy Physics, Beijing, P. R. China), Z. L. Hou(Institute of High Energy Physics, Beijing, P. R. China), H. M. Hu(Institute of High Energy Physics, Beijing, P. R. China), J. F. Hu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), T. Hu(Institute of High Energy Physics, Beijing, P. R. China), B. Huang(Institute of High Energy Physics, Beijing, P. R. China), G. M. Huang(Huazhong Normal University, Wuhan, P. R. China), J. S. Huang(Henan Normal University, Xinxiang, P. R. China), X. T. Huang(Shandong University, Jinan, P. R. China), Y. P. Huang(Institute of High Energy Physics, Beijing, P. R. China), T. Hussain(University of the Punjab, Lahore, Pakistan), C. S. Ji(University of Science and Technology of China, Hefei, P. R. China), Q. Ji(Institute of High Energy Physics, Beijing, P. R. China), X. B. Ji(Institute of High Energy Physics, Beijing, P. R. China), X. L. Ji(Institute of High Energy Physics, Beijing, P. R. China), L. K. Jia(Institute of High Energy Physics, Beijing, P. R. China), L. L. Jiang(Institute of High Energy Physics, Beijing, P. R. China), X. S. Jiang(Institute of High Energy Physics, Beijing, P. R. China), J. B. Jiao(Shandong University, Jinan, P. R. China), Z. Jiao(Huangshan College, Huangshan, P. R. China), D. P. Jin(Institute of High Energy Physics, Beijing, P. R. China), S. Jin(Institute of High Energy Physics, Beijing, P. R. China), F. F. Jing(Tsinghua University, Beijing, P. R. China), N. Kalantar-Nayestanaki(KVI/University of Groningen, Groningen, The Netherlands), M. Kavatsyuk(KVI/University of Groningen, Groningen, The Netherlands), W. Kuehn(Universitaet Giessen, Giessen, Germany), W. Lai(Institute of High Energy Physics, Beijing, P. R. China), J. S. Lange(Universitaet Giessen, Giessen, Germany), J. K. C. Leung(The University of Hong Kong, Pokfulam, Hong Kong), C. H. Li(Institute of High Energy Physics, Beijing, P. R. China), Cheng Li(University of Science and Technology of China, Hefei, P. R. China), Cui Li(University of Science and Technology of China, Hefei, P. R. China), D. M. Li(Zhengzhou University, Zhengzhou, P. R. China), F. Li(Institute of High Energy Physics, Beijing, P. R. China), G. Li(Institute of High Energy Physics, Beijing, P. R. China), H. B. Li(Institute of High Energy Physics, Beijing, P. R. China), J. C. Li(Institute of High Energy Physics, Beijing, P. R. China), K. Li(Hangzhou Normal University, Hangzhou, P. R. China), Lei Li(Institute of High Energy Physics, Beijing, P. R. China), N. B. Li(Nanjing Normal University, Nanjing, P. R. China), Q. J. Li(Institute of High Energy Physics, Beijing, P. R. China), S. L. Li(Institute of High Energy Physics, Beijing, P. R. China), W. D. Li(Institute of High Energy Physics, Beijing, P. R. China), W. G. Li(Institute of High Energy Physics, Beijing, P. R. China), X. L. Li(Shandong University, Jinan, P. R. China), X. N. Li(Institute of High Energy Physics, Beijing, P. R. China), X. Q. Li(Nankai University, Tianjin, P. R. China), X. R. Li(Seoul National University, Seoul, Korea), Z. B. Li(Sun Yat-Sen University, Guangzhou, P. R. China), H. Liang(University of Science and Technology of China, Hefei, P. R. China), Y. F. Liang(Sichuan University, Chengdu, P. R. China), Y. T. Liang(Universitaet Giessen, Giessen, Germany), G. R. Liao(Tsinghua University, Beijing, P. R. China), X. T. Liao(Institute of High Energy Physics, Beijing, P. R. China), B. J. Liu(Institute of High Energy Physics, Beijing, P. R. China), C. L. Liu(Carnegie Mellon University, Pittsburgh, PA, USA), C. X. Liu(Institute of High Energy Physics, Beijing, P. R. China), C. Y. Liu(Institute of High Energy Physics, Beijing, P. R. China), F. H. Liu(Shanxi University, Taiyuan, P. R. China), Fang Liu(Institute of High Energy Physics, Beijing, P. R. China), Feng Liu(Huazhong Normal University, Wuhan, P. R. China), H. Liu(Shanxi University, Taiyuan, P. R. China), H. B. Liu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), H. H. Liu(Henan University of Science and Technology, Luoyang, P. R. China), H. M. Liu(Institute of High Energy Physics, Beijing, P. R. China), H. W. Liu(Institute of High Energy Physics, Beijing, P. R. China), J. P. Liu(Wuhan University, Wuhan, P. R. China), Kun Liu(Peking University, Beijing, P. R. China), Kai Liu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), K. Y. Liu(Liaoning University, Shenyang, P. R. China), P. L. Liu(Shandong University, Jinan, P. R. China), S. B. Liu(University of Science and Technology of China, Hefei, P. R. China), X. Liu(Institute of High Energy Physics, Beijing, P. R. China), X. H. Liu(Institute of High Energy Physics, Beijing, P. R. China), Y. B. Liu(Nankai University, Tianjin, P. R. China), Y. Liu(Institute of High Energy Physics, Beijing, P. R. China), Z. A. Liu(Institute of High Energy Physics, Beijing, P. R. China), Zhiqiang Liu(Institute of High Energy Physics, Beijing, P. R. China), Zhiqing Liu(Institute of High Energy Physics, Beijing, P. R. China), H. Loehner(KVI/University of Groningen, Groningen, The Netherlands), G. R. Lu(Henan Normal University, Xinxiang, P. R. China), H. J. Lu(Huangshan College, Huangshan, P. R. China), J. G. Lu(Institute of High Energy Physics, Beijing, P. R. China), Q. W. Lu(Shanxi University, Taiyuan, P. R. China), X. R. Lu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), Y. P. Lu(Institute of High Energy Physics, Beijing, P. R. China), C. L. Luo(Nanjing Normal University, Nanjing, P. R. China), M. X. Luo(Zhejiang University, Hangzhou, P. R. China), T. Luo(University of Hawaii, Honolulu, Hawaii, USA), X. L. Luo(Institute of High Energy Physics, Beijing, P. R. China), M. Lv(Institute of High Energy Physics, Beijing, P. R. China), C. L. Ma(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), F. C. Ma(Liaoning University, Shenyang, P. R. China), H. L. Ma(Institute of High Energy Physics, Beijing, P. R. China), Q. M. Ma(Institute of High Energy Physics, Beijing, P. R. China), S. Ma(Institute of High Energy Physics, Beijing, P. R. China), T. Ma(Institute of High Energy Physics, Beijing, P. R. China), X. Y. Ma(Institute of High Energy Physics, Beijing, P. R. China), Y. Ma(Institute of High Energy Physics, Beijing, P. R. China), F. E. Maas(Helmholtz Institute Mainz, Mainz, Germany), M. Maggiora(University of Turin and INFN, Turin, Italy), Q. A. Malik(University of the Punjab, Lahore, Pakistan), H. Mao(Institute of High Energy Physics, Beijing, P. R. China), Y. J. Mao(Peking University, Beijing, P. R. China), Z. P. Mao(Institute of High Energy Physics, Beijing, P. R. China), J. G. Messchendorp(KVI/University of Groningen, Groningen, The Netherlands), J. Min(Institute of High Energy Physics, Beijing, P. R. China), T. J. Min(Institute of High Energy Physics, Beijing, P. R. China), R. E. Mitchell(Indiana University, Bloomington, Indiana, USA), X. H. Mo(Institute of High Energy Physics, Beijing, P. R. China), C. Morales Morales(Helmholtz Institute Mainz, Mainz, Germany), C. Motzko(Bochum Ruhr-University, Bochum, Germany), N. Yu. Muchnoi(G.I. Budker Institute of Nuclear Physics SB RAS), Y. Nefedov(Joint Institute for Nuclear Research, Dubna, Russia), C. Nicholson(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), I. B. Nikolaev(G.I. Budker Institute of Nuclear Physics SB RAS), Z. Ning(Institute of High Energy Physics, Beijing, P. R. China), S. L. Olsen(Seoul National University, Seoul, Korea), Q. Ouyang(Institute of High Energy Physics, Beijing, P. R. China), S. P. Pacetti(18, d), J. W. Park(Seoul National University, Seoul, Korea), M. Pelizaeus(University of Hawaii, Honolulu, Hawaii, USA), K. Peters(GSI Helmholtzcentre for Heavy Ion Research GmbH, Darmstadt, Germany), J. L. Ping(Nanjing Normal University, Nanjing, P. R. China), R. G. Ping(Institute of High Energy Physics, Beijing, P. R. China), R. Poling(University of Minnesota, Minneapolis, MN, USA), E. Prencipe(Johannes Gutenberg University of Mainz, Mainz, Germany), C. S. J. Pun(The University of Hong Kong, Pokfulam, Hong Kong), M. Qi(Nanjing University, Nanjing, P. R. China), S. Qian(Institute of High Energy Physics, Beijing, P. R. China), C. F. Qiao(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), X. S. Qin(Institute of High Energy Physics, Beijing, P. R. China), Y. Qin(Peking University, Beijing, P. R. China), Z. H. Qin(Institute of High Energy Physics, Beijing, P. R. China), J. F. Qiu(Institute of High Energy Physics, Beijing, P. R. China), K. H. Rashid(University of the Punjab, Lahore, Pakistan), G. Rong(Institute of High Energy Physics, Beijing, P. R. China), X. D. Ruan(GuangXi University, Nanning, P.R.China), A. Sarantsev(20, e), J. Schulze(Bochum Ruhr-University, Bochum, Germany), M. Shao(University of Science and Technology of China, Hefei, P. R. China), C. P. Shen(38, f), X. Y. Shen(Institute of High Energy Physics, Beijing, P. R. China), H. Y. Sheng(Institute of High Energy Physics, Beijing, P. R. China), M. R. Shepherd(Indiana University, Bloomington, Indiana, USA), X. Y. Song(Institute of High Energy Physics, Beijing, P. R. China), S. Spataro(University of Turin and INFN, Turin, Italy), B. Spruck(Universitaet Giessen, Giessen, Germany), D. H. Sun(Institute of High Energy Physics, Beijing, P. R. China), G. X. Sun(Institute of High Energy Physics, Beijing, P. R. China), J. F. Sun(Henan Normal University, Xinxiang, P. R. China), S. S. Sun(Institute of High Energy Physics, Beijing, P. R. China), X. D. Sun(Institute of High Energy Physics, Beijing, P. R. China), Y. J. Sun(University of Science and Technology of China, Hefei, P. R. China), Y. Z. Sun(Institute of High Energy Physics, Beijing, P. R. China), Z. J. Sun(Institute of High Energy Physics, Beijing, P. R. China), Z. T. Sun(University of Science and Technology of China, Hefei, P. R. China), C. J. Tang(Sichuan University, Chengdu, P. R. China), X. Tang(Institute of High Energy Physics, Beijing, P. R. China), E. H. Thorndike(University of Rochester, Rochester, New York, USA), H. L. Tian(Institute of High Energy Physics, Beijing, P. R. China), D. Toth(University of Minnesota, Minneapolis, MN, USA), M. U. Ulrich(Universitaet Giessen, Giessen, Germany), G. S. Varner(University of Hawaii, Honolulu, Hawaii, USA), B. Wang(GuangXi University, Nanning, P.R.China), B. Q. Wang(Peking University, Beijing, P. R. China), K. Wang(Institute of High Energy Physics, Beijing, P. R. China), L. L. Wang(China Center of Advanced Science and Technology, Beijing, P. R. China), L. S. Wang(Institute of High Energy Physics, Beijing, P. R. China), M. Wang(Shandong University, Jinan, P. R. China), P. Wang(Institute of High Energy Physics, Beijing, P. R. China), P. L. Wang(Institute of High Energy Physics, Beijing, P. R. China), Q. Wang(Peking University, Beijing, P. R. China), Q. J. Wang(Institute of High Energy Physics, Beijing, P. R. China), S. G. Wang(Peking University, Beijing, P. R. China), X. F. Wang(Henan Normal University, Xinxiang, P. R. China), X. L. Wang(University of Science and Technology of China, Hefei, P. R. China), Y. D. Wang(University of Science and Technology of China, Hefei, P. R. China), Y. F. Wang(Institute of High Energy Physics, Beijing, P. R. China), Y. Q. Wang(Shandong University, Jinan, P. R. China), Z. Wang(Institute of High Energy Physics, Beijing, P. R. China), Z. G. Wang(Institute of High Energy Physics, Beijing, P. R. China), Z. Y. Wang(Institute of High Energy Physics, Beijing, P. R. China), D. H. Wei(Guangxi Normal University, Guilin, P. R. China), P. Weidenkaff(Johannes Gutenberg University of Mainz, Mainz, Germany), Q. G. Wen(University of Science and Technology of China, Hefei, P. R. China), S. P. Wen(Institute of High Energy Physics, Beijing, P. R. China), M. W. Werner(Universitaet Giessen, Giessen, Germany), U. Wiedner(Bochum Ruhr-University, Bochum, Germany), L. H. Wu(Institute of High Energy Physics, Beijing, P. R. China), N. Wu(Institute of High Energy Physics, Beijing, P. R. China), S. X. Wu(University of Science and Technology of China, Hefei, P. R. China), W. Wu(Nankai University, Tianjin, P. R. China), Z. Wu(Institute of High Energy Physics, Beijing, P. R. China), L. G. Xia(Tsinghua University, Beijing, P. R. China), Z. J. Xiao(Nanjing Normal University, Nanjing, P. R. China), Y. G. Xie(Institute of High Energy Physics, Beijing, P. R. China), Q. L. Xiu(Institute of High Energy Physics, Beijing, P. R. China), G. F. Xu(Institute of High Energy Physics, Beijing, P. R. China), G. M. Xu(Peking University, Beijing, P. R. China), H. Xu(Institute of High Energy Physics, Beijing, P. R. China), Q. J. Xu(Hangzhou Normal University, Hangzhou, P. R. China), X. P. Xu(Soochow University, Suzhou, China), Y. Xu(Nankai University, Tianjin, P. R. China), Z. R. Xu(University of Science and Technology of China, Hefei, P. R. China), F. Xue(Huazhong Normal University, Wuhan, P. R. China), Z. Xue(Institute of High Energy Physics, Beijing, P. R. China), L. Yan(University of Science and Technology of China, Hefei, P. R. China), W. B. Yan(University of Science and Technology of China, Hefei, P. R. China), Y. H. Yan(Hunan University, Changsha, P. R. China), H. X. Yang(Institute of High Energy Physics, Beijing, P. R. China), T. Yang(GuangXi University, Nanning, P.R.China), Y. Yang(Huazhong Normal University, Wuhan, P. R. China), Y. X. Yang(Guangxi Normal University, Guilin, P. R. China), H. Ye(Institute of High Energy Physics, Beijing, P. R. China), M. Ye(Institute of High Energy Physics, Beijing, P. R. China), M. H. Ye(China Center of Advanced Science and Technology, Beijing, P. R. China), B. X. Yu(Institute of High Energy Physics, Beijing, P. R. China), C. X. Yu(Nankai University, Tianjin, P. R. China), J. S. Yu(Lanzhou University, Lanzhou, P. R. China), S. P. Yu(Shandong University, Jinan, P. R. China), C. Z. Yuan(Institute of High Energy Physics, Beijing, P. R. China), W. L. Yuan(Nanjing Normal University, Nanjing, P. R. China), Y. Yuan(Institute of High Energy Physics, Beijing, P. R. China), A. A. Zafar(University of the Punjab, Lahore, Pakistan), A. Z. Zallo(INFN Laboratori Nazionali di Frascati, Frascati, Italy), Y. Zeng(Hunan University, Changsha, P. R. China), B. X. Zhang(Institute of High Energy Physics, Beijing, P. R. China), B. Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), C. C. Zhang(Institute of High Energy Physics, Beijing, P. R. China), D. H. Zhang(Institute of High Energy Physics, Beijing, P. R. China), H. H. Zhang(Sun Yat-Sen University, Guangzhou, P. R. China), H. Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. Zhang(Nanjing Normal University, Nanjing, P. R. China), J. G. Zhang(Henan Normal University, Xinxiang, P. R. China), J. Q. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. W. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. Z. Zhang(Institute of High Energy Physics, Beijing, P. R. China), L. Zhang(Nanjing University, Nanjing, P. R. China), S. H. Zhang(Institute of High Energy Physics, Beijing, P. R. China), T. R. Zhang(Nanjing Normal University, Nanjing, P. R. China), X. J. Zhang(Institute of High Energy Physics, Beijing, P. R. China), X. Y. Zhang(Shandong University, Jinan, P. R. China), Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), Y. H. Zhang(Institute of High Energy Physics, Beijing, P. R. China), Y. S. Zhang(GuangXi University, Nanning, P.R.China), Z. P. Zhang(University of Science and Technology of China, Hefei, P. R. China), Z. Y. Zhang(Wuhan University, Wuhan, P. R. China), G. Zhao(Institute of High Energy Physics, Beijing, P. R. China), H. S. Zhao(Institute of High Energy Physics, Beijing, P. R. China), J. W. Zhao(Institute of High Energy Physics, Beijing, P. R. China), K. X. Zhao(Nanjing Normal University, Nanjing, P. R. China), Lei Zhao(University of Science and Technology of China, Hefei, P. R. China), Ling Zhao(Institute of High Energy Physics, Beijing, P. R. China), M. G. Zhao(Nankai University, Tianjin, P. R. China), Q. Zhao(Institute of High Energy Physics, Beijing, P. R. China), S. J. Zhao(Zhengzhou University, Zhengzhou, P. R. China), T. C. Zhao(Institute of High Energy Physics, Beijing, P. R. China), X. H. Zhao(Nanjing University, Nanjing, P. R. China), Y. B. Zhao(Institute of High Energy Physics, Beijing, P. R. China), Z. G. Zhao(University of Science and Technology of China, Hefei, P. R. China), A. Zhemchugov(20, a), B. Zheng(University of South China, Hengyang, P. R. China), J. P. Zheng(Institute of High Energy Physics, Beijing, P. R. China), Y. H. Zheng(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), Z. P. Zheng(Institute of High Energy Physics, Beijing, P. R. China), B. Zhong(Institute of High Energy Physics, Beijing, P. R. China), J. Zhong(Bochum Ruhr-University, Bochum, Germany), L. Zhou(Institute of High Energy Physics, Beijing, P. R. China), X. K. Zhou(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), X. R. Zhou(University of Science and Technology of China, Hefei, P. R. China), C. Zhu(Institute of High Energy Physics, Beijing, P. R. China), K. Zhu(Institute of High Energy Physics, Beijing, P. R. China), K. J. Zhu(Institute of High Energy Physics, Beijing, P. R. China), S. H. Zhu(Institute of High Energy Physics, Beijing, P. R. China), X. L. Zhu(Tsinghua University, Beijing, P. R. China), X. W. Zhu(Institute of High Energy Physics, Beijing, P. R. China), Y. M. Zhu(Nankai University, Tianjin, P. R. China), Y. S. Zhu(Institute of High Energy Physics, Beijing, P. R. China), Z. A. Zhu(Institute of High Energy Physics, Beijing, P. R. China), J. Zhuang(Institute of High Energy Physics, Beijing, P. R. China), B. S. Zou(Institute of High Energy Physics, Beijing, P. R. China), J. H. Zou(Institute of High Energy Physics, Beijing, P. R. China), and J. X. Zuo(Institute of High Energy Physics, Beijing, P. R. China)
Subjects: hep-ex, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The decays $J/\psi\to p\bar{p}$ and $J/\psi\to n\bar{n}$ have been investigated with a sample of 225.2 million $J/\psi$ events collected with the BESIII detector at the BEPCII $e^+e^-$ collider. The branching fractions are determined to be $\mathcal{B}(J/\psi\to p\bar{p})=(2.112\pm0.004\pm0.031)\times10^{-3}$ and $\mathcal{B}(J/\psi\to n\bar{n})=(2.07\pm0.01\pm0.17)\times10^{-3}$. Distributions of the angle $\theta$ between the proton or anti-neutron and the beam direction are well described by the form $1+\alpha\cos^2\theta$, and we find $\alpha=0.595\pm0.012\pm0.015$ for $J/\psi\to p\bar{p}$ and $\alpha=0.50\pm0.04\pm0.21$ for $J/\psi\to n\bar{n}$. Our branching-fraction results suggest a large phase angle between the strong and electromagnetic amplitudes describing the $J/\psi\to N\bar{N}$ decay.
Published: 2015

5. Two-photon widths of the $χ_{c0, 2}$ states and helicity analysis for $χ_{c2}\arγγ$}

Author: BESIII Collaboration, M. Ablikim(Institute of High Energy Physics, Beijing, P. R. China), M. N. Achasov(G.I. Budker Institute of Nuclear Physics SB RAS), D. J. Ambrose(University of Rochester, Rochester, New York, USA), F. F. An(Institute of High Energy Physics, Beijing, P. R. China), Q. An(University of Science and Technology of China, Hefei, P. R. China), Z. H. An(Institute of High Energy Physics, Beijing, P. R. China), J. Z. Bai(Institute of High Energy Physics, Beijing, P. R. China), R. B. Ferroli(INFN Laboratori Nazionali di Frascati, Frascati, Italy), Y. Ban(Peking University, Beijing, P. R. China), J. Becker(Bochum Ruhr-University, Bochum, Germany), N. Berger(Institute of High Energy Physics, Beijing, P. R. China), M. B. Bertani(INFN Laboratori Nazionali di Frascati, Frascati, Italy), J. M. Bian(University of Minnesota, Minneapolis, MN, USA), E. Boger(20, a), O. Bondarenko(KVI/University of Groningen, Groningen, The Netherlands), I. Boyko(Joint Institute for Nuclear Research, Dubna, Russia), R. A. Briere(Carnegie Mellon University, Pittsburgh, PA, USA), V. Bytev(Joint Institute for Nuclear Research, Dubna, Russia), X. Cai(Institute of High Energy Physics, Beijing, P. R. China), A. C. Calcaterra(INFN Laboratori Nazionali di Frascati, Frascati, Italy), G. F. Cao(Institute of High Energy Physics, Beijing, P. R. China), J. F. Chang(Institute of High Energy Physics, Beijing, P. R. China), G. Chelkov(20, a), G. Chen(Institute of High Energy Physics, Beijing, P. R. China), H. S. Chen(Institute of High Energy Physics, Beijing, P. R. China), J. C. Chen(Institute of High Energy Physics, Beijing, P. R. China), M. L. Chen(Institute of High Energy Physics, Beijing, P. R. China), S. J. Chen(Nanjing University, Nanjing, P. R. China), Y. Chen(Institute of High Energy Physics, Beijing, P. R. China), Y. B. Chen(Institute of High Energy Physics, Beijing, P. R. China), H. P. Cheng(Huangshan College, Huangshan, P. R. China), Y. P. Chu(Institute of High Energy Physics, Beijing, P. R. China), D. Cronin-Hennessy(University of Minnesota, Minneapolis, MN, USA), H. L. Dai(Institute of High Energy Physics, Beijing, P. R. China), J. P. Dai(Institute of High Energy Physics, Beijing, P. R. China), D. Dedovich(Joint Institute for Nuclear Research, Dubna, Russia), Z. Y. Deng(Institute of High Energy Physics, Beijing, P. R. China), A. Denig(Johannes Gutenberg University of Mainz, Mainz, Germany), I. Denysenko(20, b), M. Destefanis(University of Turin and INFN, Turin, Italy), W. M. Ding(Shandong University, Jinan, P. R. China), Y. Ding(Liaoning University, Shenyang, P. R. China), L. Y. Dong(Institute of High Energy Physics, Beijing, P. R. China), M. Y. Dong(Institute of High Energy Physics, Beijing, P. R. China), S. X. Du(Zhengzhou University, Zhengzhou, P. R. China), J. Fang(Institute of High Energy Physics, Beijing, P. R. China), S. S. Fang(Institute of High Energy Physics, Beijing, P. R. China), L. Fava(44, c), F. Feldbauer(Bochum Ruhr-University, Bochum, Germany), C. Q. Feng(University of Science and Technology of China, Hefei, P. R. China), C. D. Fu(Institute of High Energy Physics, Beijing, P. R. China), J. L. Fu(Nanjing University, Nanjing, P. R. China), Y. Gao(Tsinghua University, Beijing, P. R. China), C. Geng(University of Science and Technology of China, Hefei, P. R. China), K. Goetzen(GSI Helmholtzcentre for Heavy Ion Research GmbH, Darmstadt, Germany), W. X. Gong(Institute of High Energy Physics, Beijing, P. R. China), W. Gradl(Johannes Gutenberg University of Mainz, Mainz, Germany), M. Greco(University of Turin and INFN, Turin, Italy), M. H. Gu(Institute of High Energy Physics, Beijing, P. R. China), Y. T. Gu(GuangXi University, Nanning, P.R.China), Y. H. Guan(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), A. Q. Guo(Nankai University, Tianjin, P. R. China), L. B. Guo(Nanjing Normal University, Nanjing, P. R. China), Y. P. Guo(Nankai University, Tianjin, P. R. China), Y. L. Han(Institute of High Energy Physics, Beijing, P. R. China), X. Q. Hao(Institute of High Energy Physics, Beijing, P. R. China), F. A. Harris(University of Hawaii, Honolulu, Hawaii, USA), K. L. He(Institute of High Energy Physics, Beijing, P. R. China), M. He(Institute of High Energy Physics, Beijing, P. R. China), Z. Y. He(Nankai University, Tianjin, P. R. China), T. Held(Bochum Ruhr-University, Bochum, Germany), Y. K. Heng(Institute of High Energy Physics, Beijing, P. R. China), Z. L. Hou(Institute of High Energy Physics, Beijing, P. R. China), H. M. Hu(Institute of High Energy Physics, Beijing, P. R. China), J. F. Hu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), T. Hu(Institute of High Energy Physics, Beijing, P. R. China), B. Huang(Institute of High Energy Physics, Beijing, P. R. China), G. M. Huang(Huazhong Normal University, Wuhan, P. R. China), J. S. Huang(Henan Normal University, Xinxiang, P. R. China), X. T. Huang(Shandong University, Jinan, P. R. China), Y. P. Huang(Institute of High Energy Physics, Beijing, P. R. China), T. Hussain(University of the Punjab, Lahore, Pakistan), C. S. Ji(University of Science and Technology of China, Hefei, P. R. China), Q. Ji(Institute of High Energy Physics, Beijing, P. R. China), X. B. Ji(Institute of High Energy Physics, Beijing, P. R. China), X. L. Ji(Institute of High Energy Physics, Beijing, P. R. China), L. K. Jia(Institute of High Energy Physics, Beijing, P. R. China), L. L. Jiang(Institute of High Energy Physics, Beijing, P. R. China), X. S. Jiang(Institute of High Energy Physics, Beijing, P. R. China), J. B. Jiao(Shandong University, Jinan, P. R. China), Z. Jiao(Huangshan College, Huangshan, P. R. China), D. P. Jin(Institute of High Energy Physics, Beijing, P. R. China), S. Jin(Institute of High Energy Physics, Beijing, P. R. China), F. F. Jing(Tsinghua University, Beijing, P. R. China), N. Kalantar-Nayestanaki(KVI/University of Groningen, Groningen, The Netherlands), M. Kavatsyuk(KVI/University of Groningen, Groningen, The Netherlands), W. Kuehn(Universitaet Giessen, Giessen, Germany), W. Lai(Institute of High Energy Physics, Beijing, P. R. China), J. S. Lange(Universitaet Giessen, Giessen, Germany), J. K. C. Leung(The University of Hong Kong, Pokfulam, Hong Kong), C. H. Li(Institute of High Energy Physics, Beijing, P. R. China), Cheng Li(University of Science and Technology of China, Hefei, P. R. China), Cui Li(University of Science and Technology of China, Hefei, P. R. China), D. M. Li(Zhengzhou University, Zhengzhou, P. R. China), F. Li(Institute of High Energy Physics, Beijing, P. R. China), G. Li(Institute of High Energy Physics, Beijing, P. R. China), H. B. Li(Institute of High Energy Physics, Beijing, P. R. China), J. C. Li(Institute of High Energy Physics, Beijing, P. R. China), K. Li(Hangzhou Normal University, Hangzhou, P. R. China), Lei Li(Institute of High Energy Physics, Beijing, P. R. China), N. B. Li(Nanjing Normal University, Nanjing, P. R. China), Q. J. Li(Institute of High Energy Physics, Beijing, P. R. China), S. L. Li(Institute of High Energy Physics, Beijing, P. R. China), W. D. Li(Institute of High Energy Physics, Beijing, P. R. China), W. G. Li(Institute of High Energy Physics, Beijing, P. R. China), X. L. Li(Shandong University, Jinan, P. R. China), X. N. Li(Institute of High Energy Physics, Beijing, P. R. China), X. Q. Li(Nankai University, Tianjin, P. R. China), X. R. Li(Seoul National University, Seoul, Korea), Z. B. Li(Sun Yat-Sen University, Guangzhou, P. R. China), H. Liang(University of Science and Technology of China, Hefei, P. R. China), Y. F. Liang(Sichuan University, Chengdu, P. R. China), Y. T. Liang(Universitaet Giessen, Giessen, Germany), G. R. Liao(Tsinghua University, Beijing, P. R. China), X. T. Liao(Institute of High Energy Physics, Beijing, P. R. China), B. J. Liu(Institute of High Energy Physics, Beijing, P. R. China), C. L. Liu(Carnegie Mellon University, Pittsburgh, PA, USA), C. X. Liu(Institute of High Energy Physics, Beijing, P. R. China), C. Y. Liu(Institute of High Energy Physics, Beijing, P. R. China), F. H. Liu(Shanxi University, Taiyuan, P. R. China), Fang Liu(Institute of High Energy Physics, Beijing, P. R. China), Feng Liu(Huazhong Normal University, Wuhan, P. R. China), H. Liu(Shanxi University, Taiyuan, P. R. China), H. B. Liu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), H. H. Liu(Henan University of Science and Technology, Luoyang, P. R. China), H. M. Liu(Institute of High Energy Physics, Beijing, P. R. China), H. W. Liu(Institute of High Energy Physics, Beijing, P. R. China), J. P. Liu(Wuhan University, Wuhan, P. R. China), Kun Liu(Peking University, Beijing, P. R. China), Kai Liu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), K. Y. Liu(Liaoning University, Shenyang, P. R. China), P. L. Liu(Shandong University, Jinan, P. R. China), S. B. Liu(University of Science and Technology of China, Hefei, P. R. China), X. Liu(Institute of High Energy Physics, Beijing, P. R. China), X. H. Liu(Institute of High Energy Physics, Beijing, P. R. China), Y. B. Liu(Nankai University, Tianjin, P. R. China), Y. Liu(Institute of High Energy Physics, Beijing, P. R. China), Z. A. Liu(Institute of High Energy Physics, Beijing, P. R. China), Zhiqiang Liu(Institute of High Energy Physics, Beijing, P. R. China), Zhiqing Liu(Institute of High Energy Physics, Beijing, P. R. China), H. Loehner(KVI/University of Groningen, Groningen, The Netherlands), G. R. Lu(Henan Normal University, Xinxiang, P. R. China), H. J. Lu(Huangshan College, Huangshan, P. R. China), J. G. Lu(Institute of High Energy Physics, Beijing, P. R. China), Q. W. Lu(Shanxi University, Taiyuan, P. R. China), X. R. Lu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), Y. P. Lu(Institute of High Energy Physics, Beijing, P. R. China), C. L. Luo(Nanjing Normal University, Nanjing, P. R. China), M. X. Luo(Zhejiang University, Hangzhou, P. R. China), T. Luo(University of Hawaii, Honolulu, Hawaii, USA), X. L. Luo(Institute of High Energy Physics, Beijing, P. R. China), M. Lv(Institute of High Energy Physics, Beijing, P. R. China), C. L. Ma(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), F. C. Ma(Liaoning University, Shenyang, P. R. China), H. L. Ma(Institute of High Energy Physics, Beijing, P. R. China), Q. M. Ma(Institute of High Energy Physics, Beijing, P. R. China), S. Ma(Institute of High Energy Physics, Beijing, P. R. China), T. Ma(Institute of High Energy Physics, Beijing, P. R. China), X. Y. Ma(Institute of High Energy Physics, Beijing, P. R. China), Y. Ma(Institute of High Energy Physics, Beijing, P. R. China), F. E. Maas(Helmholtz Institute Mainz, Mainz, Germany), M. Maggiora(University of Turin and INFN, Turin, Italy), Q. A. Malik(University of the Punjab, Lahore, Pakistan), H. Mao(Institute of High Energy Physics, Beijing, P. R. China), Y. J. Mao(Peking University, Beijing, P. R. China), Z. P. Mao(Institute of High Energy Physics, Beijing, P. R. China), J. G. Messchendorp(KVI/University of Groningen, Groningen, The Netherlands), J. Min(Institute of High Energy Physics, Beijing, P. R. China), T. J. Min(Institute of High Energy Physics, Beijing, P. R. China), R. E. Mitchell(Indiana University, Bloomington, Indiana, USA), X. H. Mo(Institute of High Energy Physics, Beijing, P. R. China), C. Morales Morales(Helmholtz Institute Mainz, Mainz, Germany), C. Motzko(Bochum Ruhr-University, Bochum, Germany), N. Yu. Muchnoi(G.I. Budker Institute of Nuclear Physics SB RAS), Y. Nefedov(Joint Institute for Nuclear Research, Dubna, Russia), C. Nicholson(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), I. B. Nikolaev(G.I. Budker Institute of Nuclear Physics SB RAS), Z. Ning(Institute of High Energy Physics, Beijing, P. R. China), S. L. Olsen(Seoul National University, Seoul, Korea), Q. Ouyang(Institute of High Energy Physics, Beijing, P. R. China), S. P. Pacetti(18, d), J. W. Park(Seoul National University, Seoul, Korea), M. Pelizaeus(University of Hawaii, Honolulu, Hawaii, USA), K. Peters(GSI Helmholtzcentre for Heavy Ion Research GmbH, Darmstadt, Germany), J. L. Ping(Nanjing Normal University, Nanjing, P. R. China), R. G. Ping(Institute of High Energy Physics, Beijing, P. R. China), R. Poling(University of Minnesota, Minneapolis, MN, USA), E. Prencipe(Johannes Gutenberg University of Mainz, Mainz, Germany), C. S. J. Pun(The University of Hong Kong, Pokfulam, Hong Kong), M. Qi(Nanjing University, Nanjing, P. R. China), S. Qian(Institute of High Energy Physics, Beijing, P. R. China), C. F. Qiao(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), X. S. Qin(Institute of High Energy Physics, Beijing, P. R. China), Y. Qin(Peking University, Beijing, P. R. China), Z. H. Qin(Institute of High Energy Physics, Beijing, P. R. China), J. F. Qiu(Institute of High Energy Physics, Beijing, P. R. China), K. H. Rashid(University of the Punjab, Lahore, Pakistan), G. Rong(Institute of High Energy Physics, Beijing, P. R. China), X. D. Ruan(GuangXi University, Nanning, P.R.China), A. Sarantsev(20, e), J. Schulze(Bochum Ruhr-University, Bochum, Germany), M. Shao(University of Science and Technology of China, Hefei, P. R. China), C. P. Shen(38, f), X. Y. Shen(Institute of High Energy Physics, Beijing, P. R. China), H. Y. Sheng(Institute of High Energy Physics, Beijing, P. R. China), M. R. Shepherd(Indiana University, Bloomington, Indiana, USA), X. Y. Song(Institute of High Energy Physics, Beijing, P. R. China), S. Spataro(University of Turin and INFN, Turin, Italy), B. Spruck(Universitaet Giessen, Giessen, Germany), D. H. Sun(Institute of High Energy Physics, Beijing, P. R. China), G. X. Sun(Institute of High Energy Physics, Beijing, P. R. China), J. F. Sun(Henan Normal University, Xinxiang, P. R. China), S. S. Sun(Institute of High Energy Physics, Beijing, P. R. China), X. D. Sun(Institute of High Energy Physics, Beijing, P. R. China), Y. J. Sun(University of Science and Technology of China, Hefei, P. R. China), Y. Z. Sun(Institute of High Energy Physics, Beijing, P. R. China), Z. J. Sun(Institute of High Energy Physics, Beijing, P. R. China), Z. T. Sun(University of Science and Technology of China, Hefei, P. R. China), C. J. Tang(Sichuan University, Chengdu, P. R. China), X. Tang(Institute of High Energy Physics, Beijing, P. R. China), E. H. Thorndike(University of Rochester, Rochester, New York, USA), H. L. Tian(Institute of High Energy Physics, Beijing, P. R. China), D. Toth(University of Minnesota, Minneapolis, MN, USA), M. U. Ulrich(Universitaet Giessen, Giessen, Germany), G. S. Varner(University of Hawaii, Honolulu, Hawaii, USA), B. Wang(GuangXi University, Nanning, P.R.China), B. Q. Wang(Peking University, Beijing, P. R. China), K. Wang(Institute of High Energy Physics, Beijing, P. R. China), L. L. Wang(China Center of Advanced Science and Technology, Beijing, P. R. China), L. S. Wang(Institute of High Energy Physics, Beijing, P. R. China), M. Wang(Shandong University, Jinan, P. R. China), P. Wang(Institute of High Energy Physics, Beijing, P. R. China), P. L. Wang(Institute of High Energy Physics, Beijing, P. R. China), Q. Wang(Peking University, Beijing, P. R. China), Q. J. Wang(Institute of High Energy Physics, Beijing, P. R. China), S. G. Wang(Peking University, Beijing, P. R. China), X. F. Wang(Henan Normal University, Xinxiang, P. R. China), X. L. Wang(University of Science and Technology of China, Hefei, P. R. China), Y. D. Wang(University of Science and Technology of China, Hefei, P. R. China), Y. F. Wang(Institute of High Energy Physics, Beijing, P. R. China), Y. Q. Wang(Shandong University, Jinan, P. R. China), Z. Wang(Institute of High Energy Physics, Beijing, P. R. China), Z. G. Wang(Institute of High Energy Physics, Beijing, P. R. China), Z. Y. Wang(Institute of High Energy Physics, Beijing, P. R. China), D. H. Wei(Guangxi Normal University, Guilin, P. R. China), P. Weidenkaff(Johannes Gutenberg University of Mainz, Mainz, Germany), Q. G. Wen(University of Science and Technology of China, Hefei, P. R. China), S. P. Wen(Institute of High Energy Physics, Beijing, P. R. China), M. W. Werner(Universitaet Giessen, Giessen, Germany), U. Wiedner(Bochum Ruhr-University, Bochum, Germany), L. H. Wu(Institute of High Energy Physics, Beijing, P. R. China), N. Wu(Institute of High Energy Physics, Beijing, P. R. China), S. X. Wu(University of Science and Technology of China, Hefei, P. R. China), W. Wu(Nankai University, Tianjin, P. R. China), Z. Wu(Institute of High Energy Physics, Beijing, P. R. China), L. G. Xia(Tsinghua University, Beijing, P. R. China), Z. J. Xiao(Nanjing Normal University, Nanjing, P. R. China), Y. G. Xie(Institute of High Energy Physics, Beijing, P. R. China), Q. L. Xiu(Institute of High Energy Physics, Beijing, P. R. China), G. F. Xu(Institute of High Energy Physics, Beijing, P. R. China), G. M. Xu(Peking University, Beijing, P. R. China), H. Xu(Institute of High Energy Physics, Beijing, P. R. China), Q. J. Xu(Hangzhou Normal University, Hangzhou, P. R. China), X. P. Xu(Soochow University, Suzhou, China), Y. Xu(Nankai University, Tianjin, P. R. China), Z. R. Xu(University of Science and Technology of China, Hefei, P. R. China), F. Xue(Huazhong Normal University, Wuhan, P. R. China), Z. Xue(Institute of High Energy Physics, Beijing, P. R. China), L. Yan(University of Science and Technology of China, Hefei, P. R. China), W. B. Yan(University of Science and Technology of China, Hefei, P. R. China), Y. H. Yan(Hunan University, Changsha, P. R. China), H. X. Yang(Institute of High Energy Physics, Beijing, P. R. China), T. Yang(GuangXi University, Nanning, P.R.China), Y. Yang(Huazhong Normal University, Wuhan, P. R. China), Y. X. Yang(Guangxi Normal University, Guilin, P. R. China), H. Ye(Institute of High Energy Physics, Beijing, P. R. China), M. Ye(Institute of High Energy Physics, Beijing, P. R. China), M. H. Ye(China Center of Advanced Science and Technology, Beijing, P. R. China), B. X. Yu(Institute of High Energy Physics, Beijing, P. R. China), C. X. Yu(Nankai University, Tianjin, P. R. China), J. S. Yu(Lanzhou University, Lanzhou, P. R. China), S. P. Yu(Shandong University, Jinan, P. R. China), C. Z. Yuan(Institute of High Energy Physics, Beijing, P. R. China), W. L. Yuan(Nanjing Normal University, Nanjing, P. R. China), Y. Yuan(Institute of High Energy Physics, Beijing, P. R. China), A. A. Zafar(University of the Punjab, Lahore, Pakistan), A. Z. Zallo(INFN Laboratori Nazionali di Frascati, Frascati, Italy), Y. Zeng(Hunan University, Changsha, P. R. China), B. X. Zhang(Institute of High Energy Physics, Beijing, P. R. China), B. Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), C. C. Zhang(Institute of High Energy Physics, Beijing, P. R. China), D. H. Zhang(Institute of High Energy Physics, Beijing, P. R. China), H. H. Zhang(Sun Yat-Sen University, Guangzhou, P. R. China), H. Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. Zhang(Nanjing Normal University, Nanjing, P. R. China), J. G. Zhang(Henan Normal University, Xinxiang, P. R. China), J. Q. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. W. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. Z. Zhang(Institute of High Energy Physics, Beijing, P. R. China), L. Zhang(Nanjing University, Nanjing, P. R. China), S. H. Zhang(Institute of High Energy Physics, Beijing, P. R. China), T. R. Zhang(Nanjing Normal University, Nanjing, P. R. China), X. J. Zhang(Institute of High Energy Physics, Beijing, P. R. China), X. Y. Zhang(Shandong University, Jinan, P. R. China), Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), Y. H. Zhang(Institute of High Energy Physics, Beijing, P. R. China), Y. S. Zhang(GuangXi University, Nanning, P.R.China), Z. P. Zhang(University of Science and Technology of China, Hefei, P. R. China), Z. Y. Zhang(Wuhan University, Wuhan, P. R. China), G. Zhao(Institute of High Energy Physics, Beijing, P. R. China), H. S. Zhao(Institute of High Energy Physics, Beijing, P. R. China), J. W. Zhao(Institute of High Energy Physics, Beijing, P. R. China), K. X. Zhao(Nanjing Normal University, Nanjing, P. R. China), Lei Zhao(University of Science and Technology of China, Hefei, P. R. China), Ling Zhao(Institute of High Energy Physics, Beijing, P. R. China), M. G. Zhao(Nankai University, Tianjin, P. R. China), Q. Zhao(Institute of High Energy Physics, Beijing, P. R. China), S. J. Zhao(Zhengzhou University, Zhengzhou, P. R. China), T. C. Zhao(Institute of High Energy Physics, Beijing, P. R. China), X. H. Zhao(Nanjing University, Nanjing, P. R. China), Y. B. Zhao(Institute of High Energy Physics, Beijing, P. R. China), Z. G. Zhao(University of Science and Technology of China, Hefei, P. R. China), A. Zhemchugov(20, a), B. Zheng(University of South China, Hengyang, P. R. China), J. P. Zheng(Institute of High Energy Physics, Beijing, P. R. China), Y. H. Zheng(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), Z. P. Zheng(Institute of High Energy Physics, Beijing, P. R. China), B. Zhong(Institute of High Energy Physics, Beijing, P. R. China), J. Zhong(Bochum Ruhr-University, Bochum, Germany), L. Zhou(Institute of High Energy Physics, Beijing, P. R. China), X. K. Zhou(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), X. R. Zhou(University of Science and Technology of China, Hefei, P. R. China), C. Zhu(Institute of High Energy Physics, Beijing, P. R. China), K. Zhu(Institute of High Energy Physics, Beijing, P. R. China), K. J. Zhu(Institute of High Energy Physics, Beijing, P. R. China), S. H. Zhu(Institute of High Energy Physics, Beijing, P. R. China), X. L. Zhu(Tsinghua University, Beijing, P. R. China), X. W. Zhu(Institute of High Energy Physics, Beijing, P. R. China), Y. M. Zhu(Nankai University, Tianjin, P. R. China), Y. S. Zhu(Institute of High Energy Physics, Beijing, P. R. China), Z. A. Zhu(Institute of High Energy Physics, Beijing, P. R. China), J. Zhuang(Institute of High Energy Physics, Beijing, P. R. China), B. S. Zou(Institute of High Energy Physics, Beijing, P. R. China), J. H. Zou(Institute of High Energy Physics, Beijing, P. R. China), and J. X. Zuo(Institute of High Energy Physics, Beijing, P. R. China)
Subjects: hep-ex, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Based on a data sample of 106 M $\psi^{\prime}$ events collected with the BESIII detector, the decays $\psi^{\prime}\ar\gamma\chi_{c0, 2}$,$\chi_{c0, 2}\ar\gamma\gamma$ are studied to determine the two-photon widths of the $\chi_{c0, 2}$ states. The two-photon decay branching fractions are determined to be ${\cal B}(\chi_{c0}\ar\gamma\gamma) = (2.24\pm 0.19\pm 0.12\pm 0.08)\times 10^{-4}$ and ${\cal B}(\chi_{c2}\ar\gamma\gamma) = (3.21\pm 0.18\pm 0.17\pm 0.13)\times 10^{-4}$. From these, the two-photon widths are determined to be $\Gamma_{\gamma \gamma}(\chi_{c0}) = (2.33\pm0.20\pm0.13\pm0.17)$ keV, $\Gamma_{\gamma \gamma}(\chi_{c2}) = (0.63\pm0.04\pm0.04\pm0.04)$ keV, and $\cal R$ $=\Gamma_{\gamma \gamma}(\chi_{c2})/\Gamma_{\gamma \gamma}(\chi_{c0})=0.271\pm 0.029\pm 0.013\pm 0.027$, where the uncertainties are statistical, systematic, and those from the PDG ${\cal B}(\psi^{\prime}\ar\gamma\chi_{c0,2})$ and $\Gamma(\chi_{c0,2})$ errors, respectively. The ratio of the two-photon widths for helicity $\lambda=0$ and helicity $\lambda=2$ components in the decay $\chi_{c2}\ar\gamma\gamma$ is measured for the first time to be $f_{0/2} =\Gamma^{\lambda=0}_{\gamma\gamma}(\chi_{c2})/\Gamma^{\lambda=2}_{\gamma\gamma}(\chi_{c2}) = 0.00\pm0.02\pm0.02$.
Published: 2015

6. Could electron-positron annihilation lines in the Galactic center result from pulsar winds?

Author: C. S. J. Pun, K. S. Cheng, and Wei Wang
Subjects: Physics, education.field_of_study, Astrophysics::High Energy Astrophysical Phenomena, Electron–positron annihilation, Astrophysics (astro-ph), Population, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Magnetar, Neutron star, Positron, Pulsar, Space and Planetary Science, Millisecond pulsar, education, Gamma-ray burst
Abstract: we study the possibility of pulsar winds in the Galactic center (GC) to produce the 511 keV line. We propose that there may exist three possible scenarios of pulsar winds as the positron sources: normal pulsars; rapidly spinning strongly magnetized neutron stars in GRB progenitors; a population of millisecond pulsars in the Galactic center region. These $e^\pm$pairs could be trapped in the region by the magnetic field in the GC, and cool through the synchrotron radiation and Coulomb interactions with the medium. The cooling timescales are lower than the diffuse timescale of positrons, so low energy positrons could annihilate directly with electrons into 511 keV photons or form positronium before annihilation. We find that normal pulsars cannot be a significant contributor to the positron sources. Although magnetars in the GC could be potential sources of positrons, their birth rate and birth locations may impose some problems for this scenario. We believe that the most likely candidate positron sources in the GC may be a population of millisecond pulsars in the GC. Our preliminary estimations predict the e$^\pm$ annihilation rate in the GC is $> 5\times 10^{42}$ s$^{-1}$. Therefore, the $e^\pm$ pairs from pulsars winds can contribute significantly to the positron sources in the GC. Furthermore, since the diffusion length of positrons is short, we predict that the intensity distribution of the annihilation line should follow the distribution of millisecond pulsars, which should correlate to the mass distribution in the GC., 7 pages, A&A in press
Published: 2006
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7. The Axisymmetric Ejecta of Supernova 1987A

Author: Nino Panagia, Richard McCray, Dietrich Baade, Peter Hoeflich, A. M. Khokhlov, P. M. Garnavich, P. Challis, George Sonneborn, C. S. J. Pun, N. B. Suntzeff, David Branch, Peter Lundqvist, Claes Fransson, M. M. Phillips, Alexei V. Filippenko, Lingyu Wang, R. P. Kirshner, and John C Wheeler
Subjects: Physics, media_common.quotation_subject, Astronomy and Astrophysics, Astrophysics, Polarization (waves), 01 natural sciences, Spectral line, Redshift, symbols.namesake, Supernova, Space and Planetary Science, Sky, 0103 physical sciences, symbols, 010306 general physics, Axial symmetry, Ejecta, 010303 astronomy & astrophysics, Doppler effect, media_common
Abstract: to the plane of the sky. We also demonstratethat the polarization represents a prolate geometry with the same position angleand axis as the early speckle data and the late-time image and hence that thegeometry has been ﬁxed in time and throughout the ejecta. The Bochum eventand the Doppler kinematics of the [Ca II]/[O II] emission in spatially resolvedHST spectra of the ejecta can be consistently integrated into this geometry. Theradioactive clump is deduced to fall approximately along the axis of the innercircumstellar ring and therefore to be redshifted in the North whereas the [CaII]/[O II] 7300 ˚A emission is redshifted in the South. We present a jet-induc edmodel for the explosion and argue that such a model can account for many of
Published: 2002
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8. 56Ni Mixing in the Outer Layers of SN 1987A

Author: E. Baron, C. S. J. Pun, Peter H. Hauschildt, Sergei Blinnikov, Robert C. Mitchell, Peter Lundqvist, and David Branch
Subjects: Nuclear reaction, Physics, 010308 nuclear & particles physics, Balmer series, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, symbols.namesake, Supernova, Space and Planetary Science, Nucleosynthesis, 0103 physical sciences, symbols, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Mixing (physics), Envelope (waves)
Abstract: Supernova 1987A remains the most well observed and well studied supernova to date. Observations have produced excellent broadband photometric and spectroscopic coverage over a wide wavelength range at all epochs. Here we focus on the very early spectroscopic observations. Only recently have numerical models been of sufficient detail to accurately explain the observed spectra. In SN 1987A, good agreement has been found between observed and synthetic spectra for day 1, but by day 4, the predicted Balmer lines become much weaker than the observed lines. We present the results of work based on a radiation-hydrodynamic model by Blinnikov and collaborators. Synthetic non-LTE spectra generated from this model by the general radiation transfer code PHOENIX strongly support the theory that significant mixing of 56Ni into the outer envelope is required to maintain strong Balmer lines. Preliminary results suggest a lower limit to the average nickel mass of 1.0 × 10-5 M☉ is required above 5000 km s-1 by day 4. PHOENIX models thus have the potential to be a sensitive probe for nickel mixing in the outer layers of a supernova.
Published: 2001
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9. Analysis of Type IIn SN 1998S: Effects of Circumstellar Interaction on Observed Spectra

Author: Claes Fransson, Nate Bastian, Peter M. Garnavich, Brian P. Schmidt, E. Michael, Nino Panagia, R. P. Kirshner, Bruno Leibundgut, Richard McCray, Alexei V. Filippenko, Eric J. Lentz, Lingyu Wang, John C Wheeler, C. S. J. Pun, Peter Lundqvist, Peter H. Hauschildt, M. M. Phillips, Saurabh Jha, David Branch, E. Baron, P. Challis, George Sonneborn, and N. B. Suntzeff
Subjects: Physics, 010308 nuclear & particles physics, Thermodynamic equilibrium, Astrophysics::High Energy Astrophysical Phenomena, Order (ring theory), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Type (model theory), 01 natural sciences, Spectral line, Atmosphere, Supernova, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectral analysis, Ejecta, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present spectral analysis of early observations of the Type IIn supernova 1998S using the general non-local thermodynamic equilibrium atmosphere code \tt PHOENIX}. We model both the underlying supernova spectrum and the overlying circumstellar interaction region and produce spectra in good agreement with observations. The early spectra are well fit by lines produced primarily in the circumstellar region itself, and later spectra are due primarily to the supernova ejecta. Intermediate spectra are affected by both regions. A mass-loss rate of order $\dot M \sim 0.0001-0.001$\msol yr$^{-1}$ is inferred for a wind speed of 100-1000 \kmps. We discuss how future self-consistent models will better clarify the underlying progenitor structure.
Published: 2001
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10. [ITAL]Hubble Space Telescope[/ITAL] Spectroscopy of Spot 1 on the Circumstellar Ring of SN 1987A

Author: John C. Raymond, Kazimierz J. Borkowski, George Sonneborn, Richard McCray, Mark M. Phillips, Peter Challis, Lifan Wang, C. S. J. Pun, Roger A. Chevalier, Alexei V. Filippenko, Claes Fransson, Robert P. Kirshner, J. Craig Wheeler, Peter Lundqvist, Nino Panagia, Peter M. Garnavich, Eli Michael, and Nicholas B. Suntzeff
Subjects: Shock wave, Physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectral line, Supernova, Bright spot, Space and Planetary Science, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, Spectroscopy, Astrophysics::Galaxy Astrophysics, Space Telescope Imaging Spectrograph, Line (formation)
Abstract: We present ultraviolet and optical spectra of the first bright spot (P.A. = 29°) on SN 1987A's equatorial circumstellar ring taken with the Space Telescope Imaging Spectrograph. We interpret this spot as the emission produced by radiative shocks that occur where the supernova blast wave strikes an inward protrusion of the ring. The observed line widths and intensity ratios indicate the presence of radiative shocks with velocities ranging from 100 to 250 km s-1 entering dense (104 cm-3) gas. These observations, and future observations of the development of the spectra and line profiles, provide a unique opportunity to study the hydrodynamics of radiative shocks.
Published: 2000
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11. High-Velocity L[CLC]y[/CLC]α Emission from SNR 1987A

Author: Eli Michael, George Sonneborn, C. S. J. Pun, Richard McCray, and Kazimierz J. Borkowski
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radius, Plasma, Shock (mechanics), Luminosity, Radial velocity, Supernova, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Space Telescope Imaging Spectrograph, Envelope (waves)
Abstract: The high-velocity Lya emission from SN 1987A observed with the Space Telescope Imaging Spectrograph (STIS) evidently comes from a reverse shock formed where the outer envelope of SN 1987A strikes ionized gas inside the inner circumstellar ring. The observations can be explained by a simple kinematic model, in which the Lya emission comes from hydrogen atoms with radial velocity »15,000 km s 21 crossing a reverse shock in the shape of a slightly prolate ellipsoid with equatorial radius cm or »80% of the distance to the 17 4.8 # 10 inner surface of the inner ring. N v ll1239, 1243 emission, if present, has a net luminosity &30% times that of the Lya emission. Future STIS observations should enable us to predict the time of impact with the inner ring and to determine unambiguously whether or not N v emission is present. These observations will offer a unique opportunity to probe the structure of SN 1987A’s circumstellar environment and the hydrodynamics and kinetics of very fast shocks. Subject heading: circumstellar matter — hydrodynamics — supernovae: individual (SN 1987A) — ultraviolet: ISM
Published: 1998
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12. Observation of two new N* resonances in the decay ψ(3686)→ppπ0

Author: M, Ablikim, M N, Achasov, D J, Ambrose, F F, An, Q, An, Z H, An, J Z, Bai, Y, Ban, J, Becker, N, Berger, M, Bertani, J M, Bian, E, Boger, O, Bondarenko, I, Boyko, R A, Briere, V, Bytev, X, Cai, A, Calcaterra, G F, Cao, J F, Chang, G, Chelkov, G, Chen, H S, Chen, J C, Chen, M L, Chen, S J, Chen, Y, Chen, Y B, Chen, H P, Cheng, Y P, Chu, D, Cronin-Hennessy, H L, Dai, J P, Dai, D, Dedovich, Z Y, Deng, A, Denig, I, Denysenko, M, Destefanis, W M, Ding, Y, Ding, L Y, Dong, M Y, Dong, S X, Du, J, Fang, S S, Fang, L, Fava, F, Feldbauer, C Q, Feng, R B, Ferroli, C D, Fu, J L, Fu, Y, Gao, C, Geng, K, Goetzen, W X, Gong, W, Gradl, M, Greco, M H, Gu, Y T, Gu, Y H, Guan, A Q, Guo, L B, Guo, Y P, Guo, Y L, Han, X Q, Hao, F A, Harris, K L, He, M, He, Z Y, He, T, Held, Y K, Heng, Z L, Hou, H M, Hu, J F, Hu, T, Hu, B, Huang, G M, Huang, J S, Huang, X T, Huang, Y P, Huang, T, Hussain, C S, Ji, Q, Ji, X B, Ji, X L, Ji, L K, Jia, L L, Jiang, X S, Jiang, J B, Jiao, Z, Jiao, D P, Jin, S, Jin, F F, Jing, N, Kalantar-Nayestanaki, M, Kavatsyuk, W, Kühn, W, Lai, J S, Lange, J K C, Leung, C H, Li, Cheng, Li, Cui, Li, D M, Li, F, Li, G, Li, H B, Li, J C, Li, K, Li, Lei, Li, N B, Li, Q J, Li, S L, Li, W D, Li, W G, Li, X L, Li, X N, Li, X Q, Li, X R, Li, Z B, Li, H, Liang, Y F, Liang, Y T, Liang, G R, Liao, X T, Liao, B J, Liu, C L, Liu, C X, Liu, C Y, Liu, F H, Liu, Fang, Liu, Feng, Liu, H, Liu, H B, Liu, H H, Liu, H M, Liu, H W, Liu, J P, Liu, K Y, Liu, Kai, Liu, Kun, Liu, P L, Liu, S B, Liu, X, Liu, X H, Liu, Y, Liu, Y B, Liu, Z A, Liu, Zhiqiang, Liu, Zhiqing, Liu, H, Loehner, G R, Lu, H J, Lu, J G, Lu, Q W, Lu, X R, Lu, Y P, Lu, C L, Luo, M X, Luo, T, Luo, X L, Luo, M, Lv, C L, Ma, F C, Ma, H L, Ma, Q M, Ma, S, Ma, T, Ma, X Y, Ma, Y, Ma, F E, Maas, M, Maggiora, Q A, Malik, H, Mao, Y J, Mao, Z P, Mao, J G, Messchendorp, J, Min, T J, Min, R E, Mitchell, X H, Mo, C, Morales Morales, C, Motzko, N Yu, Muchnoi, Y, Nefedov, C, Nicholson, I B, Nikolaev, Z, Ning, S L, Olsen, Q, Ouyang, S, Pacetti, J W, Park, M, Pelizaeus, K, Peters, J L, Ping, R G, Ping, R, Poling, E, Prencipe, C S J, Pun, M, Qi, S, Qian, C F, Qiao, X S, Qin, Y, Qin, Z H, Qin, J F, Qiu, K H, Rashid, G, Rong, X D, Ruan, A, Sarantsev, J, Schulze, M, Shao, C P, Shen, X Y, Shen, H Y, Sheng, M R, Shepherd, X Y, Song, S, Spataro, B, Spruck, D H, Sun, G X, Sun, J F, Sun, S S, Sun, X D, Sun, Y J, Sun, Y Z, Sun, Z J, Sun, Z T, Sun, C J, Tang, X, Tang, E H, Thorndike, H L, Tian, D, Toth, M, Ullrich, G S, Varner, B, Wang, B Q, Wang, J X, Wang, K, Wang, L L, Wang, L S, Wang, M, Wang, P, Wang, P L, Wang, Q, Wang, Q J, Wang, S G, Wang, X F, Wang, X L, Wang, Y D, Wang, Y F, Wang, Y Q, Wang, Z, Wang, Z G, Wang, Z Y, Wang, D H, Wei, P, Weidenkaff, Q G, Wen, S P, Wen, M, Werner, U, Wiedner, L H, Wu, N, Wu, S X, Wu, W, Wu, Z, Wu, L G, Xia, Z J, Xiao, Y G, Xie, Q L, Xiu, G F, Xu, G M, Xu, H, Xu, Q J, Xu, X P, Xu, Y, Xu, Z R, Xu, F, Xue, Z, Xue, L, Yan, W B, Yan, Y H, Yan, H X, Yang, T, Yang, Y, Yang, Y X, Yang, H, Ye, M, Ye, M H, Ye, B X, Yu, C X, Yu, J S, Yu, S P, Yu, C Z, Yuan, W L, Yuan, Y, Yuan, A A, Zafar, A, Zallo, Y, Zeng, B X, Zhang, B Y, Zhang, C C, Zhang, D H, Zhang, H H, Zhang, H Y, Zhang, J, Zhang, J G, Zhang, J Q, Zhang, J W, Zhang, J Y, Zhang, J Z, Zhang, L, Zhang, S H, Zhang, T R, Zhang, X J, Zhang, X Y, Zhang, Y, Zhang, Y H, Zhang, Y S, Zhang, Z P, Zhang, Z Y, Zhang, G, Zhao, H S, Zhao, J W, Zhao, K X, Zhao, Lei, Zhao, Ling, Zhao, M G, Zhao, Q, Zhao, S J, Zhao, T C, Zhao, X H, Zhao, Y B, Zhao, Z G, Zhao, A, Zhemchugov, B, Zheng, J P, Zheng, Y H, Zheng, Z P, Zheng, B, Zhong, J, Zhong, L, Zhou, X K, Zhou, X R, Zhou, C, Zhu, K, Zhu, K J, Zhu, S H, Zhu, X L, Zhu, X W, Zhu, Y M, Zhu, Y S, Zhu, Z A, Zhu, J, Zhuang, B S, Zou, J H, Zou, and J X, Zuo
Abstract: Based on 106×10(6)ψ(3686) events collected with the BESIII detector at the BEPCII facility, a partial wave analysis of ψ(3686)→ppπ0 is performed. The branching fraction of this channel has been determined to be B(ψ(3686)→ppπ0)=(1.65±0.03±0.15)×10(-4). In this decay, 7 N* intermediate resonances are observed. Among these, two new resonances, N(2300) and N(2570) are significant, one 1/2+ resonance with a mass of 2300(-30-0)(+40+109) MeV/c2 and width of 340(-30-58)(+30+110) MeV/c2, and one 5/2- resonance with a mass of 2570(-10-10)(+19+34) MeV/c2 and width of 250(-24-21)(+14+69) MeV/c2. For the remaining 5 N* intermediate resonances [N(1440), N(1520), N(1535), N(1650) and N(1720)], the analysis yields mass and width values that are consistent with those from established resonances.
Published: 2012

13. Evidence for the direct two-photon transition from ψ(3686) to J/ψ

Author: M, Ablikim, M N, Achasov, D J, Ambrose, F F, An, Q, An, Z H, An, J Z, Bai, R B, Ferroli, Y, Ban, J, Becker, N, Berger, M B, Bertani, J M, Bian, E, Boger, O, Bondarenko, I, Boyko, R A, Briere, V, Bytev, X, Cai, A C, Calcaterra, G F, Cao, J F, Chang, G, Chelkov, G, Chen, H S, Chen, J C, Chen, M L, Chen, S J, Chen, Y, Chen, Y B, Chen, H P, Cheng, Y P, Chu, D, Cronin-Hennessy, H L, Dai, J P, Dai, D, Dedovich, Z Y, Deng, A, Denig, I, Denysenko, M, Destefanis, W M, Ding, Y, Ding, L Y, Dong, M Y, Dong, S X, Du, J, Fang, S S, Fang, L, Fava, F, Feldbauer, C Q, Feng, C D, Fu, J L, Fu, Y, Gao, C, Geng, K, Goetzen, W X, Gong, W, Gradl, M, Greco, M H, Gu, Y T, Gu, Y H, Guan, A Q, Guo, L B, Guo, Y P, Guo, Y L, Han, X Q, Hao, F A, Harris, K L, He, M, He, Z Y, He, T, Held, Y K, Heng, Z L, Hou, H M, Hu, J F, Hu, T, Hu, B, Huang, G M, Huang, J S, Huang, X T, Huang, Y P, Huang, T, Hussain, C S, Ji, Q, Ji, X B, Ji, X L, Ji, L K, Jia, L L, Jiang, X S, Jiang, J B, Jiao, Z, Jiao, D P, Jin, S, Jin, F F, Jing, N, Kalantar-Nayestanaki, M, Kavatsyuk, W, Kuehn, W, Lai, J S, Lange, J K C, Leung, C H, Li, Cheng, Li, Cui, Li, D M, Li, F, Li, G, Li, H B, Li, J C, Li, K, Li, Lei, Li, N B, Li, Q J, Li, S L, Li, W D, Li, W G, Li, X L, Li, X N, Li, X Q, Li, X R, Li, Z B, Li, H, Liang, Y F, Liang, Y T, Liang, G R, Liao, X T, Liao, B J, Liu, C L, Liu, C X, Liu, C Y, Liu, F H, Liu, Fang, Liu, Feng, Liu, H, Liu, H B, Liu, H H, Liu, H M, Liu, H W, Liu, J P, Liu, Kun, Liu, Kai, Liu, K Y, Liu, P L, Liu, S B, Liu, X, Liu, X H, Liu, Y B, Liu, Y, Liu, Z A, Liu, Zhiqiang, Liu, Zhiqing, Liu, H, Loehner, G R, Lu, H J, Lu, J G, Lu, Q W, Lu, X R, Lu, Y P, Lu, C L, Luo, M X, Luo, T, Luo, X L, Luo, M, Lv, C L, Ma, F C, Ma, H L, Ma, Q M, Ma, S, Ma, T, Ma, X Y, Ma, Y, Ma, F E, Maas, M, Maggiora, Q A, Malik, H, Mao, Y J, Mao, Z P, Mao, J G, Messchendorp, J, Min, T J, Min, R E, Mitchell, X H, Mo, C, Morales Morales, C, Motzko, N Yu, Muchnoi, Y, Nefedov, C, Nicholson, I B, Nikolaev, Z, Ning, S L, Olsen, Q, Ouyang, S P, Pacetti, J W, Park, M, Pelizaeus, K, Peters, J L, Ping, R G, Ping, R, Poling, E, Prencipe, C S J, Pun, M, Qi, S, Qian, C F, Qiao, X S, Qin, Y, Qin, Z H, Qin, J F, Qiu, K H, Rashid, G, Rong, X D, Ruan, A, Sarantsev, J, Schulze, M, Shao, C P, Shen, X Y, Shen, H Y, Sheng, M R, Shepherd, X Y, Song, S, Spataro, B, Spruck, D H, Sun, G X, Sun, J F, Sun, S S, Sun, X D, Sun, Y J, Sun, Y Z, Sun, Z J, Sun, Z T, Sun, C J, Tang, X, Tang, E H, Thorndike, H L, Tian, D, Toth, M U, Ulrich, G S, Varner, B, Wang, B Q, Wang, K, Wang, L L, Wang, L S, Wang, M, Wang, P, Wang, P L, Wang, Q, Wang, Q J, Wang, S G, Wang, X F, Wang, X L, Wang, Y D, Wang, Y F, Wang, Y Q, Wang, Z, Wang, Z G, Wang, Z Y, Wang, D H, Wei, P, Weidenkaff, Q G, Wen, S P, Wen, M W, Werner, U, Wiedner, L H, Wu, N, Wu, S X, Wu, W, Wu, Z, Wu, L G, Xia, Z J, Xiao, Y G, Xie, Q L, Xiu, G F, Xu, G M, Xu, H, Xu, Q J, Xu, X P, Xu, Y, Xu, Z R, Xu, F, Xue, Z, Xue, L, Yan, W B, Yan, Y H, Yan, H X, Yang, T, Yang, Y, Yang, Y X, Yang, H, Ye, M, Ye, M H, Ye, B X, Yu, C X, Yu, J S, Yu, S P, Yu, C Z, Yuan, W L, Yuan, Y, Yuan, A A, Zafar, A Z, Zallo, Y, Zeng, B X, Zhang, B Y, Zhang, C C, Zhang, D H, Zhang, H H, Zhang, H Y, Zhang, J, Zhang, J G, Zhang, J Q, Zhang, J W, Zhang, J Y, Zhang, J Z, Zhang, L, Zhang, S H, Zhang, T R, Zhang, X J, Zhang, X Y, Zhang, Y, Zhang, Y H, Zhang, Y S, Zhang, Z P, Zhang, Z Y, Zhang, G, Zhao, H S, Zhao, J W, Zhao, K X, Zhao, Lei, Zhao, Ling, Zhao, M G, Zhao, Q, Zhao, S J, Zhao, T C, Zhao, X H, Zhao, Y B, Zhao, Z G, Zhao, A, Zhemchugov, B, Zheng, J P, Zheng, Y H, Zheng, Z P, Zheng, B, Zhong, J, Zhong, L, Zhou, X K, Zhou, X R, Zhou, C, Zhu, K, Zhu, K J, Zhu, S H, Zhu, X L, Zhu, X W, Zhu, Y M, Zhu, Y S, Zhu, Z A, Zhu, J, Zhuang, B S, Zou, J H, Zou, and J X, Zuo
Subjects: Physics, Particle physics, Branching fraction, Electron–positron annihilation, General Physics and Astronomy
Abstract: The two-photon transition ψ(3686)→γγJ/ψ is studied in a sample of 1.06×10(8) ψ(3686) decays collected by the BESIII detector. The branching fraction is measured to be (3.1±0.6(stat)(-1.0)(+0.8)(syst))×10(-4) using J/ψ→e(+)e(-) and J/ψ→μ(+)μ(-) decays, and its upper limit is estimated to be 4.5×10(-4) at the 90% confidence level. This work represents the first measurement of a two-photon transition among charmonium states. The orientation of the ψ(3686) decay plane and the J/ψ polarization in this decay are also studied. In addition, the product branching fractions of sequential E1 transitions ψ(3686)→γχ(cJ) and χ(cJ)→γJ/ψ(J=0,1,2) are reported.
Published: 2012

14. ηπ+ π- resonant structure around 1.8 GeV/c(2) and η(1405) in J/ψ → ωηπ+ π

Author: M, Ablikim, M N, Achasov, D, Alberto, Q, An, Z H, An, J Z, Bai, R, Baldini, Y, Ban, J, Becker, N, Berger, M, Bertani, J M, Bian, O, Bondarenko, I, Boyko, R A, Briere, V, Bytev, X, Cai, A C, Calcaterra, G F, Cao, X X, Cao, J F, Chang, G, Chelkov, G, Chen, H S, Chen, J C, Chen, M L, Chen, S J, Chen, Y, Chen, Y B, Chen, H P, Cheng, Y P, Chu, D, Cronin-Hennessy, H L, Dai, J P, Dai, D, Dedovich, Z Y, Deng, I, Denysenko, M, Destefanis, Y, Ding, L Y, Dong, M Y, Dong, S X, Du, R R, Fan, J, Fang, S S, Fang, C Q, Feng, C D, Fu, J L, Fu, Y, Gao, C, Geng, K, Goetzen, W X, Gong, M, Greco, S, Grishin, M H, Gu, Y T, Gu, Y H, Guan, A Q, Guo, L B, Guo, Y P, Guo, X Q, Hao, F A, Harris, K L, He, M, He, Z Y, He, Y K, Heng, Z L, Hou, H M, Hu, J F, Hu, T, Hu, B, Huang, G M, Huang, J S, Huang, X T, Huang, Y P, Huang, T, Hussain, C S, Ji, Q, Ji, X B, Ji, X L, Ji, L K, Jia, L L, Jiang, X S, Jiang, J B, Jiao, Z, Jiao, D P, Jin, S, Jin, F F, Jing, N, Kalantar-Nayestanaki, M, Kavatsyuk, S, Komamiya, W, Kuehn, J S, Lange, J K C, Leung, Cheng, Li, Cui, Li, D M, Li, F, Li, G, Li, H B, Li, J C, Li, K, Li, Lei, Li, N B, Li, Q J, Li, W D, Li, W G, Li, X L, Li, X N, Li, X Q, Li, X R, Li, Z B, Li, H, Liang, Y F, Liang, Y T, Liang, X T, Liao, B J, Liu, C L, Liu, C X, Liu, C Y, Liu, F H, Liu, Fang, Liu, Feng, Liu, G C, Liu, H, Liu, H B, Liu, H H, Liu, H M, Liu, H W, Liu, J P, Liu, K, Liu, K Y, Liu, Q, Liu, S B, Liu, X, Liu, X H, Liu, Y B, Liu, Y W, Liu, Yong, Liu, Z A, Liu, Z Q, Liu, H, Loehner, G R, Lu, H J, Lu, J G, Lu, Q W, Lu, X R, Lu, Y P, Lu, C L, Luo, M X, Luo, T, Luo, X L, Luo, C L, Ma, F C, Ma, H L, Ma, Q M, Ma, T, Ma, X, Ma, X Y, Ma, M, Maggiora, Q A, Malik, H, Mao, Y J, Mao, Z P, Mao, J G, Messchendorp, J, Min, R E, Mitchell, X H, Mo, N Yu, Muchnoi, Y, Nefedov, I B, Nikolaev, Z, Ning, S L, Olsen, Q, Ouyang, S, Pacetti, M, Pelizaeus, K, Peters, J L, Ping, R G, Ping, R, Poling, C S J, Pun, M, Qi, S, Qian, C F, Qiao, X S, Qin, J F, Qiu, K H, Rashid, G, Rong, X D, Ruan, A, Sarantsev, J, Schulze, M, Shao, C P, Shen, X Y, Shen, H Y, Sheng, M R, Shepherd, X Y, Song, S, Sonoda, S, Spataro, B, Spruck, D H, Sun, G X, Sun, J F, Sun, S S, Sun, X D, Sun, Y J, Sun, Y Z, Sun, Z J, Sun, Z T, Sun, C J, Tang, X, Tang, H L, Tian, D, Toth, G S, Varner, X, Wan, B Q, Wang, K, Wang, L L, Wang, L S, Wang, M, Wang, P, Wang, P L, Wang, Q, Wang, S G, Wang, X L, Wang, Y D, Wang, Y F, Wang, Y Q, Wang, Z, Wang, Z G, Wang, Z Y, Wang, D H, Wei, Q G, Wen, S P, Wen, U, Wiedner, L H, Wu, N, Wu, W, Wu, Z, Wu, Z J, Xiao, Y G, Xie, G F, Xu, G M, Xu, H, Xu, Q J, Xu, X P, Xu, Y, Xu, Z R, Xu, Z Z, Xu, Z, Xue, L, Yan, W B, Yan, Y H, Yan, H X, Yang, M, Yang, T, Yang, Y, Yang, Y X, Yang, M, Ye, M H, Ye, B X, Yu, C X, Yu, L, Yu, S P Yu, Yu, C Z, Yuan, W L, Yuan, Y, Yuan, A A, Zafar, A, Zallo, Y, Zeng, B X, Zhang, B Y, Zhang, C C, Zhang, D H, Zhang, H H, Zhang, H Y, Zhang, J, Zhang, J W, Zhang, J Y, Zhang, J Z, Zhang, L, Zhang, S H, Zhang, T R, Zhang, X J, Zhang, X Y, Zhang, Y, Zhang, Y H, Zhang, Z P, Zhang, Z Y, Zhang, G, Zhao, H S, Zhao, Jiawei, Zhao, Jingwei, Zhao, Lei, Zhao, Ling, Zhao, M G, Zhao, Q, Zhao, S J, Zhao, T C, Zhao, X H, Zhao, Y B, Zhao, Z G, Zhao, Z L, Zhao, A, Zhemchugov, B, Zheng, J P, Zheng, Y H, Zheng, Z P, Zheng, B, Zhong, J, Zhong, L, Zhong, L, Zhou, X K, Zhou, X R, Zhou, C, Zhu, K, Zhu, K J, Zhu, S H, Zhu, X L, Zhu, X W, Zhu, Y S, Zhu, Z A, Zhu, J, Zhuang, B S, Zou, J H, Zou, and J X, Zuo
Abstract: We present results of a study of the decay J/ψ → ωηπ+ π- using a sample of (225.2 ± 2.8) × 10(6) J/ψ events collected by the BESIII detector, and report the observation of a new process J/ψ → ωX(1870) with a statistical significance of 7.2σ, in which X(1870) decays to a(0)(±)(980)π±. Fitting to ηπ+ π- mass spectrum yields a mass M = 1877.3 ± 6.3(stat)(-7.4)(+3.4)(syst) MeV/c(2), a width Γ = 57 ± 12(stat)(-4)(+19)(syst) MeV/c(2), and a product branching fraction B(J/ψ → ωX) × B(X→a(0)(±)(980)π±) × B(a(0) (±)(980) → ηπ±) = [1.50 ± 0.26(stat)(-0.36)(+0.72) (syst)] × 10(-4). Signals for J/ψ → ωf(1)(1285) and J/ψ → ω η(1405) are also clearly observed and measured.
Published: 2011

15. Observation of χ(c1) decays into vector meson pairs φφ, ωω, and ωφ

Author: M, Ablikim, M N, Achasov, L, An, Q, An, Z H, An, J Z, Bai, R, Baldini, Y, Ban, J, Becker, N, Berger, M, Bertani, J M, Bian, O, Bondarenko, I, Boyko, R A, Briere, V, Bytev, X, Cai, G F, Cao, X X, Cao, J F, Chang, G, Chelkov, G, Chen, H S, Chen, J C, Chen, M L, Chen, S J, Chen, Y, Chen, Y B, Chen, H P, Cheng, Y P, Chu, D, Cronin-Hennessy, H L, Dai, J P, Dai, D, Dedovich, Z Y, Deng, I, Denysenko, M, Destefanis, Y, Ding, L Y, Dong, M Y, Dong, S X, Du, M Y, Duan, R R, Fan, J, Fang, S S, Fang, C Q, Feng, C D, Fu, J L, Fu, Y, Gao, C, Geng, K, Goetzen, W X, Gong, M, Greco, S, Grishin, M H, Gu, Y T, Gu, Y H, Guan, A Q, Guo, L B, Guo, Y P, Guo, X Q, Hao, F A, Harris, K L, He, M, He, Z Y, He, Y K, Heng, Z L, Hou, H M, Hu, J F, Hu, T, Hu, B, Huang, G M, Huang, J S, Huang, X T, Huang, Y P, Huang, T, Hussain, C S, Ji, Q, Ji, X B, Ji, X L, Ji, L K, Jia, L L, Jiang, X S, Jiang, J B, Jiao, Z, Jiao, D P, Jin, S, Jin, F F, Jing, M, Kavatsyuk, S, Komamiya, W, Kuehn, J S, Lange, J K C, Leung, Cheng, Li, Cui, Li, D M, Li, F, Li, G, Li, H B, Li, J C, Li, Lei, Li, N B, Li, Q J, Li, W D, Li, W G, Li, X L, Li, X N, Li, X Q, Li, X R, Li, Z B, Li, H, Liang, Y F, Liang, Y T, Liang, G R, Liao, X T, Liao, B J, Liu, C L, Liu, C X, Liu, C Y, Liu, F H, Liu, Fang, Liu, Feng, Liu, G C, Liu, H, Liu, H B, Liu, H M, Liu, H W, Liu, J P, Liu, K, Liu, K Y, Liu, Q, Liu, S B, Liu, X, Liu, X H, Liu, Y B, Liu, Y W, Liu, Yong, Liu, Z A, Liu, Z Q, Liu, H, Loehner, G R, Lu, H J, Lu, J G, Lu, Q W, Lu, X R, Lu, Y P, Lu, C L, Luo, M X, Luo, T, Luo, X L, Luo, C L, Ma, F C, Ma, H L, Ma, Q M, Ma, T, Ma, X, Ma, X Y, Ma, M, Maggiora, Q A, Malik, H, Mao, Y J, Mao, Z P, Mao, J G, Messchendorp, J, Min, R E, Mitchell, X H, Mo, N Yu, Muchnoi, Y, Nefedov, Z, Ning, S L, Olsen, Q, Ouyang, S, Pacetti, M, Pelizaeus, K, Peters, J L, Ping, R G, Ping, R, Poling, C S J, Pun, M, Qi, S, Qian, C F, Qiao, X S, Qin, J F, Qiu, K H, Rashid, G, Rong, X D, Ruan, A, Sarantsev, J, Schulze, M, Shao, C P, Shen, X Y, Shen, H Y, Sheng, M R, Shepherd, X Y, Song, S, Sonoda, S, Spataro, B, Spruck, D H, Sun, G X, Sun, J F, Sun, S S, Sun, X D, Sun, Y J, Sun, Y Z, Sun, Z J, Sun, Z T, Sun, C J, Tang, X, Tang, X F, Tang, H L, Tian, D, Toth, G S, Varner, X, Wan, B Q, Wang, K, Wang, L L, Wang, L S, Wang, M, Wang, P, Wang, P L, Wang, Q, Wang, S G, Wang, X L, Wang, Y D, Wang, Y F, Wang, Y Q, Wang, Z, Wang, Z G, Wang, Z Y, Wang, D H, Wei, Q G, Wen, S P, Wen, U, Wiedner, L H, Wu, N, Wu, W, Wu, Z, Wu, Z J, Xiao, Y G, Xie, G F, Xu, G M, Xu, H, Xu, Y, Xu, Z R, Xu, Z Z, Xu, Z, Xue, L, Yan, W B, Yan, Y H, Yan, H X, Yang, M, Yang, T, Yang, Y, Yang, Y X, Yang, M, Ye, M H, Ye, B X, Yu, C X, Yu, L, Yu, C Z, Yuan, W L, Yuan, Y, Yuan, A A, Zafar, A, Zallo, Y, Zeng, B X, Zhang, B Y, Zhang, C C, Zhang, D H, Zhang, H H, Zhang, H Y, Zhang, J, Zhang, J W, Zhang, J Y, Zhang, J Z, Zhang, L, Zhang, S H, Zhang, T R, Zhang, X J, Zhang, X Y, Zhang, Y, Zhang, Y H, Zhang, Z P, Zhang, Z Y, Zhang, G, Zhao, H S, Zhao, Jiawei, Zhao, Jingwei, Zhao, Lei, Zhao, Ling, Zhao, M G, Zhao, Q, Zhao, S J, Zhao, T C, Zhao, X H, Zhao, Y B, Zhao, Z G, Zhao, Z L, Zhao, A, Zhemchugov, B, Zheng, J P, Zheng, Y H, Zheng, Z P, Zheng, B, Zhong, J, Zhong, L, Zhong, L, Zhou, X K, Zhou, X R, Zhou, C, Zhu, K, Zhu, K J, Zhu, S H, Zhu, X L, Zhu, X W, Zhu, Y S, Zhu, Z A, Zhu, J, Zhuang, B S, Zou, J H, Zou, J X, Zuo, and P, Zweber
Abstract: Using (106±4)×10⁻⁶ ψ(3686) events accumulated with the BESIII detector at the BEPCII e⁺e⁻ collider, we present the first measurement of decays of χ(c1) to vector meson pairs φφ, ωω, and ωφ. The branching fractions are measured to be (4.4±0.3±0.5)×10⁻⁴, (6.0±0.3±0.7)×10⁻⁴, and (2.2±0.6±0.2)×10⁻⁵, for χ(c1)→φφ, ωω, and ωφ, respectively, which indicates that the hadron helicity selection rule is significantly violated in χ(cJ) decays. In addition, the measurement of χ(cJ)→ωφ provides the first indication of the rate of doubly OZI-suppressed χ(cJ) decay. Finally, we present improved measurements for the branching fractions of χ(c0) and χ(c2) to vector meson pairs.
Published: 2011

16. Confirmation of the X(1835) and Observation of the Resonances X(2120) and X(2370) in J/ψ→γπ+π-η′

Author: M, Ablikim, M N, Achasov, L, An, Q, An, Z H, An, J Z, Bai, R, Baldini, Y, Ban, J, Becker, N, Berger, M, Bertani, J M, Bian, I, Boyko, R A, Briere, V, Bytev, X, Cai, G F, Cao, X X, Cao, J F, Chang, G, Chelkov, G, Chen, H S, Chen, J C, Chen, M L, Chen, S J, Chen, Y, Chen, Y B, Chen, H P, Cheng, Y P, Chu, D, Cronin-Hennessy, H L, Dai, J P, Dai, D, Dedovich, Z Y, Deng, I, Denysenko, M, Destefanis, Y, Ding, L Y, Dong, M Y, Dong, S X, Du, M Y, Duan, R R, Fan, J, Fang, S S, Fang, F, Feldbauer, C Q, Feng, C D, Fu, J L, Fu, Y, Gao, C, Geng, K, Goetzen, W X, Gong, M, Greco, S, Grishin, M H, Gu, Y T, Gu, Y H, Guan, A Q, Guo, L B, Guo, Y P, Guo, X Q, Hao, F A, Harris, K L, He, M, He, Z Y, He, Y K, Heng, Z L, Hou, H M, Hu, J F, Hu, T, Hu, B, Huang, G M, Huang, J S, Huang, X T, Huang, Y P, Huang, T, Hussain, C S, Ji, Q, Ji, X B, Ji, X L, Ji, L K, Jia, L L, Jiang, X S, Jiang, J B, Jiao, Z, Jiao, D P, Jin, S, Jin, F F, Jing, M, Kavatsyuk, S, Komamiya, W, Kuehn, J S, Lange, J K C, Leung, Cheng, Li, Cui, Li, D M, Li, F, Li, G, Li, H B, Li, J C, Li, Lei, Li, N B, Li, Q J, Li, W D, Li, W G, Li, X L, Li, X N, Li, X Q, Li, X R, Li, Z B, Li, H, Liang, Y F, Liang, Y T, Liang, G R, Liao, X T, Liao, B J, Liu, C L, Liu, C X, Liu, C Y, Liu, F H, Liu, Fang, Liu, Feng, Liu, G C, Liu, H, Liu, H B, Liu, H M, Liu, H W, Liu, J P, Liu, K, Liu, K Y, Liu, Q, Liu, S B, Liu, X, Liu, X H, Liu, Y B, Liu, Y W, Liu, Yong, Liu, Z A, Liu, Z Q, Liu, H, Loehner, G R, Lu, H J, Lu, J G, Lu, Q W, Lu, X R, Lu, Y P, Lu, C L, Luo, M X, Luo, T, Luo, X L, Luo, C L, Ma, F C, Ma, H L, Ma, Q M, Ma, T, Ma, X, Ma, X Y, Ma, M, Maggiora, Q A, Malik, H, Mao, Y J, Mao, Z P, Mao, J G, Messchendorp, J, Min, R E, Mitchell, X H, Mo, C, Motzko, N Yu, Muchnoi, Y, Nefedov, Z, Ning, S L, Olsen, Q, Ouyang, S, Pacetti, M, Pelizaeus, K, Peters, J L, Ping, R G, Ping, R, Poling, C S J, Pun, M, Qi, S, Qian, C F, Qiao, X S, Qin, J F, Qiu, K H, Rashid, G, Rong, X D, Ruan, A, Sarantsev, J, Schulze, M, Shao, C P, Shen, X Y, Shen, H Y, Sheng, M R, Shepherd, X Y, Song, S, Sonoda, S, Spataro, B, Spruck, D H, Sun, G X, Sun, J F, Sun, S S, Sun, X D, Sun, Y J, Sun, Y Z, Sun, Z J, Sun, Z T, Sun, C J, Tang, X, Tang, X F, Tang, H L, Tian, D, Toth, G S, Varner, X, Wan, B Q, Wang, K, Wang, L L, Wang, L S, Wang, M, Wang, P, Wang, P L, Wang, Q, Wang, S G, Wang, X L, Wang, Y D, Wang, Y F, Wang, Y Q, Wang, Z, Wang, Z G, Wang, Z Y, Wang, D H, Wei, S P, Wen, U, Wiedner, L H, Wu, N, Wu, W, Wu, Z, Wu, Z J, Xiao, Y G, Xie, G F, Xu, G M, Xu, H, Xu, Y, Xu, Z R, Xu, Z Z, Xu, Z, Xue, L, Yan, W B, Yan, Y H, Yan, H X, Yang, M, Yang, T, Yang, Y, Yang, Y X, Yang, M, Ye, M H, Ye, B X, Yu, C X, Yu, L, Yu, C Z, Yuan, W L, Yuan, Y, Yuan, A A, Zafar, A, Zallo, Y, Zeng, B X, Zhang, B Y, Zhang, C C, Zhang, D H, Zhang, H H, Zhang, H Y, Zhang, J, Zhang, J W, Zhang, J Y, Zhang, J Z, Zhang, L, Zhang, S H, Zhang, T R, Zhang, X J, Zhang, X Y, Zhang, Y, Zhang, Y H, Zhang, Z P, Zhang, Z Y, Zhang, G, Zhao, H S, Zhao, Jiawei, Zhao, Jingwei, Zhao, Lei, Zhao, Ling, Zhao, M G, Zhao, Q, Zhao, S J, Zhao, T C, Zhao, X H, Zhao, Y B, Zhao, Z G, Zhao, Z L, Zhao, A, Zhemchugov, B, Zheng, J P, Zheng, Y H, Zheng, Z P, Zheng, B, Zhong, J, Zhong, L, Zhong, L, Zhou, X K, Zhou, X R, Zhou, C, Zhu, K, Zhu, K J, Zhu, S H, Zhu, X L, Zhu, X W, Zhu, Y S, Zhu, Z A, Zhu, J, Zhuang, B S, Zou, J H, Zou, J X, Zuo, and P, Zweber
Subjects: BARYONIUM, GLUEBALL
Abstract: With a sample of (225.2±2.8)×10(6) J/ψ events registered in the BESIII detector, J/ψ→γπ(+)π(-)η(') is studied using two η(') decay modes: η(')→π(+)π(-)η and η(')→γρ(0). The X(1835), which was previously observed by BESII, is confirmed with a statistical significance that is larger than 20σ. In addition, in the π(+)π(-)η(') invariant-mass spectrum, the X(2120) and the X(2370), are observed with statistical significances larger than 7.2σ and 6.4σ, respectively. For the X(1835), the angular distribution of the radiative photon is consistent with expectations for a pseudoscalar.
Published: 2011

17. X-ray illumination of the ejecta of supernova 1987A

Author: J. Larsson, C. Fransson, G. Östlin, P. Gröningsson, A. Jerkstrand, C. Kozma, J. Sollerman, P. Challis, R. P. Kirshner, R. A. Chevalier, K. Heng, R. McCray, N. B. Suntzeff, P. Bouchet, A. Crotts, J. Danziger, E. Dwek, K. France, P. M. Garnavich, S. S. Lawrence, B. Leibundgut, P. Lundqvist, N. Panagia, C. S. J. Pun, N. Smith, G. Sonneborn, L. Wang, J. C. Wheeler, Oskar Klein Centre [Stockholm], Stockholm University, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Department of Astronomy [Charlottesville], University of Virginia, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Joint Institute for Laboratory Astrophysics (JILA), National Institute of Standards and Technology [Gaithersburg] (NIST)-University of Colorado [Boulder], George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University [College Station], Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Astronomy, Columbia University [New York], INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), NASA Goddard Space Flight Center (GSFC), Center for Astrophysics and Space Astronomy [Boulder] (CASA), University of Colorado [Boulder], 225 Nieuwland Science, University of Notre Dame [Indiana] (UND), Department of Physics and Astronomy, Hofstra University [Hempstead], European Southern Observatory (ESO), Space Telescope Science Institute (STSci), Department of Physics, The University of Hong Kong (HKU), Steward observatory, University of Arizona, Imagerie et modélisation Vasculaires, Thoraciques et Cérébrales (MOTIVATE), Centre de Recherche en Acquisition et Traitement de l'Image pour la Santé (CREATIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [Austin], University of Texas at Austin [Austin], Savelli, Bruno, Harvard University [Cambridge]-Smithsonian Institution, Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Hospices Civils de Lyon (HCL)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Hospices Civils de Lyon (HCL)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), University of Virginia [Charlottesville], Université Jean Monnet [Saint-Étienne] (UJM)-Hospices Civils de Lyon (HCL)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Jean Monnet [Saint-Étienne] (UJM)-Hospices Civils de Lyon (HCL)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), and Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)
Subjects: Milky Way, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, [SPI.SIGNAL] Engineering Sciences [physics]/Signal and Image processing, Physics, Multidisciplinary, 010308 nuclear & particles physics, Astronomy, Light curve, Near-Earth supernova, Supernova, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, [SPI.SIGNAL]Engineering Sciences [physics]/Signal and Image processing, Radioactive decay
Abstract: We present the late-time optical light curve of the ejecta of SN 1987A measured from HST imaging observations spanning the past 17 years. We find that the flux from the ejecta declined up to around year 2001, powered by the radioactive decay of 44Ti. Then the flux started to increase, more than doubling by the end of 2009. We show that the increase is the result of energy deposited by X-rays produced in the interaction with the circumstellar medium. We suggest that the change of the dominant energy input to the ejecta, from internal to external, marks the transition from supernova to supernova remnant. The details of the observations and the modelling are described in the accompanying supplementary information., To appear in Nature on 23 June 2011 (already available online). 39 pages with 10 figures
Published: 2011
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18. Evidence forψ′Decays intoγπ0andγη

Author: M. Ablikim, M. N. Achasov, L. An, Q. An, Z. H. An, J. Z. Bai, R. Baldini, Y. Ban, J. Becker, N. Berger, M. Bertani, J. M. Bian, I. Boyko, R. A. Briere, V. Bytev, X. Cai, G. F. Cao, X. X. Cao, J. F. Chang, G. Chelkov, G. Chen, H. S. Chen, J. C. Chen, M. L. Chen, S. J. Chen, Y. Chen, Y. B. Chen, H. P. Cheng, Y. P. Chu, D. Cronin-Hennessy, H. L. Dai, J. P. Dai, D. Dedovich, Z. Y. Deng, I. Denysenko, M. Destefanis, Y. Ding, L. Y. Dong, M. Y. Dong, S. X. Du, M. Y. Duan, R. R. Fan, J. Fang, S. S. Fang, F. Feldbauer, C. Q. Feng, C. D. Fu, J. L. Fu, Y. Gao, C. Geng, K. Goetzen, W. X. Gong, M. Greco, S. Grishin, M. H. Gu, Y. T. Gu, Y. H. Guan, A. Q. Guo, L. B. Guo, Y. P. Guo, X. Q. Hao, F. A. Harris, K. L. He, M. He, Z. Y. He, Y. K. Heng, Z. L. Hou, H. M. Hu, J. F. Hu, T. Hu, B. Huang, G. M. Huang, J. S. Huang, X. T. Huang, Y. P. Huang, T. Hussain, C. S. Ji, Q. Ji, X. B. Ji, X. L. Ji, L. K. Jia, L. L. Jiang, X. S. Jiang, J. B. Jiao, Z. Jiao, D. P. Jin, S. Jin, F. F. Jing, M. Kavatsyuk, S. Komamiya, W. Kuehn, J. S. Lange, J. K. C. Leung, Cheng Li, Cui Li, D. M. Li, F. Li, G. Li, H. B. Li, J. C. Li, Lei Li, N. B. Li, Q. J. Li, W. D. Li, W. G. Li, X. L. Li, X. N. Li, X. Q. Li, X. R. Li, Z. B. Li, H. Liang, Y. F. Liang, Y. T. Liang, G. R. Liao, X. T. Liao, B. J. Liu, C. L. Liu, C. X. Liu, C. Y. Liu, F. H. Liu, Fang Liu, Feng Liu, G. C. Liu, H. Liu, H. B. Liu, H. M. Liu, H. W. Liu, J. P. Liu, K. Liu, K. Y. Liu, Q. Liu, S. B. Liu, X. H. Liu, Y. B. Liu, Y. W. Liu, Yong Liu, Z. A. Liu, Z. Q. Liu, H. Loehner, G. R. Lu, H. J. Lu, J. G. Lu, Q. W. Lu, X. R. Lu, Y. P. Lu, C. L. Luo, M. X. Luo, T. Luo, X. L. Luo, C. L. Ma, F. C. Ma, H. L. Ma, Q. M. Ma, T. Ma, X. Ma, X. Y. Ma, M. Maggiora, Q. A. Malik, H. Mao, Y. J. Mao, Z. P. Mao, J. G. Messchendorp, J. Min, R. E. Mitchell, X. H. Mo, C. Motzko, N. Yu. Muchnoi, Y. Nefedov, Z. Ning, S. L. Olsen, Q. Ouyang, S. Pacetti, M. Pelizaeus, K. Peters, J. L. Ping, R. G. Ping, R. Poling, C. S. J. Pun, M. Qi, S. Qian, C. F. Qiao, X. S. Qin, J. F. Qiu, K. H. Rashid, G. Rong, X. D. Ruan, A. Sarantsev, J. Schulze, M. Shao, C. P. Shen, X. Y. Shen, H. Y. Sheng, M. R. Shepherd, X. Y. Song, S. Sonoda, S. Spataro, B. Spruck, D. H. Sun, G. X. Sun, J. F. Sun, S. S. Sun, X. D. Sun, Y. J. Sun, Y. Z. Sun, Z. J. Sun, Z. T. Sun, C. J. Tang, X. Tang, X. F. Tang, H. L. Tian, D. Toth, G. S. Varner, X. Wan, B. Q. Wang, K. Wang, L. L. Wang, L. S. Wang, P. Wang, P. L. Wang, Q. Wang, S. G. Wang, X. L. Wang, Y. D. Wang, Y. F. Wang, Y. Q. Wang, Z. Wang, Z. G. Wang, Z. Y. Wang, D. H. Wei, S. P. Wen, U. Wiedner, L. H. Wu, N. Wu, W. Wu, Z. Wu, Z. J. Xiao, Y. G. Xie, G. F. Xu, G. M. Xu, H. Xu, Y. Xu, Z. R. Xu, Z. Z. Xu, Z. Xue, L. Yan, W. B. Yan, Y. H. Yan, H. X. Yang, M. Yang, T. Yang, Y. Yang, Y. X. Yang, M. Ye, M. H. Ye, B. X. Yu, C. X. Yu, L. Yu, C. Z. Yuan, W. L. Yuan, Y. Yuan, A. A. Zafar, A. Zallo, Y. Zeng, B. X. Zhang, B. Y. Zhang, C. C. Zhang, D. H. Zhang, H. H. Zhang, H. Y. Zhang, J. Zhang, J. W. Zhang, J. Y. Zhang, J. Z. Zhang, L. Zhang, S. H. Zhang, T. R. Zhang, X. J. Zhang, X. Y. Zhang, Y. Zhang, Y. H. Zhang, Z. P. Zhang, Z. Y. Zhang, G. Zhao, H. S. Zhao, Jiawei Zhao, Jingwei Zhao, Lei Zhao, Ling Zhao, M. G. Zhao, Q. Zhao, S. J. Zhao, T. C. Zhao, X. H. Zhao, Y. B. Zhao, Z. G. Zhao, Z. L. Zhao, A. Zhemchugov, B. Zheng, J. P. Zheng, Y. H. Zheng, Z. P. Zheng, B. Zhong, J. Zhong, L. Zhong, L. Zhou, X. K. Zhou, X. R. Zhou, C. Zhu, K. Zhu, K. J. Zhu, S. H. Zhu, X. L. Zhu, X. W. Zhu, Y. S. Zhu, Z. A. Zhu, J. Zhuang, B. S. Zou, J. H. Zou, J. X. Zuo, and P. Zweber
Subjects: Physics, General Physics and Astronomy
Published: 2010
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19. Measurements of h(c)(1P(1)) in psi' decays

Author: M, Ablikim, M N, Achasov, L, An, Q, An, Z H, An, J Z, Bai, Y, Ban, N, Berger, J M, Bian, I, Boyko, R A, Briere, V, Bytev, X, Cai, G F, Cao, X X, Cao, J F, Chang, G, Chelkov, G, Chen, H S, Chen, J C, Chen, L P, Chen, M L, Chen, P, Chen, S J, Chen, Y B, Chen, Y P, Chu, D, Cronin-Hennessy, H L, Dai, J P, Dai, D, Dedovich, Z Y, Deng, I, Denysenko, M, Destefanis, Y, Ding, L Y, Dong, M Y, Dong, S X, Du, M Y, Duan, J, Fang, C Q, Feng, C D, Fu, J L, Fu, Y, Gao, C, Geng, K, Goetzen, W X, Gong, M, Greco, S, Grishin, Y T, Gu, A Q, Guo, L B, Guo, Y P, Guo, S Q, Han, F A, Harris, K L, He, M, He, Z Y, He, Y K, Heng, Z L, Hou, H M, Hu, J F, Hu, T, Hu, X W, Hu, B, Huang, G M, Huang, J S, Huang, X T, Huang, Y P, Huang, C S, Ji, Q, Ji, X B, Ji, X L, Ji, L K, Jia, L L, Jiang, X S, Jiang, J B, Jiao, D P, Jin, S, Jin, S, Komamiya, W, Kuehn, S, Lange, J K C, Leung, Cheng, Li, Cui, Li, D M, Li, F, Li, G, Li, H B, Li, J, Li, J C, Li, Lei, Li, Lu, Li, Q J, Li, W D, Li, W G, Li, X L, Li, X N, Li, X Q, Li, X R, Li, Y X, Li, Z B, Li, H, Liang, T R, Liang, Y T, Liang, Y F, Liang, G R, Liao, X T, Liao, B J, Liu, C L, Liu, C X, Liu, C Y, Liu, F H, Liu, Fang, Liu, Feng, Liu, G C, Liu, H, Liu, H B, Liu, H M, Liu, H W, Liu, J, Liu, J P, Liu, K, Liu, K Y, Liu, Q, Liu, S B, Liu, X H, Liu, Y B, Liu, Y F, Liu, Y W, Liu, Yong, Liu, Z A, Liu, G R, Lu, J G, Lu, Q W, Lu, X R, Lu, Y P, Lu, C L, Luo, M X, Luo, T, Luo, X L, Luo, C L, Ma, F C, Ma, H L, Ma, Q M, Ma, X, Ma, X Y, Ma, M, Maggiora, Y J, Mao, Z P, Mao, J, Min, X H, Mo, N Yu, Muchnoi, Y, Nefedov, F P, Ning, S L, Olsen, Q, Ouyang, M, Pelizaeus, K, Peters, J L, Ping, R G, Ping, R, Poling, C S J, Pun, M, Qi, S, Qian, C F, Qiao, J F, Qiu, G, Rong, X D, Ruan, A, Sarantsev, M, Shao, C P, Shen, X Y, Shen, H Y, Sheng, S, Sonoda, S, Spataro, B, Spruck, D H, Sun, G X, Sun, J F, Sun, S S, Sun, X D, Sun, Y J, Sun, Y Z, Sun, Z J, Sun, Z T, Sun, C J, Tang, X, Tang, X F, Tang, H L, Tian, D, Toth, G S, Varner, X, Wan, B Q, Wang, J K, Wang, K, Wang, L L, Wang, L S, Wang, P, Wang, P L, Wang, Q, Wang, S G, Wang, X D, Wang, X L, Wang, Y D, Wang, Y F, Wang, Y Q, Wang, Z, Wang, Z G, Wang, Z Y, Wang, D H, Wei, S P, Wen, U, Wiedner, L H, Wu, N, Wu, W, Wu, Y M, Wu, Z, Wu, Z J, Xiao, Y G, Xie, G F, Xu, G M, Xu, H, Xu, Min, Xu, Ming, Xu, X P, Xu, Y, Xu, Z Z, Xu, Z, Xue, L, Yan, W B, Yan, Y H, Yan, H X, Yang, M, Yang, P, Yang, S M, Yang, Y X, Yang, M, Ye, M H, Ye, B X, Yu, C X, Yu, L, Yu, C Z, Yuan, Y, Yuan, Y, Zeng, B X, Zhang, B Y, Zhang, C C, Zhang, D H, Zhang, H H, Zhang, H Y, Zhang, J W, Zhang, J Y, Zhang, J Z, Zhang, L, Zhang, S H, Zhang, X Y, Zhang, Y, Zhang, Y H, Zhang, Z P, Zhang, C, Zhao, H S, Zhao, Jiawei, Zhao, Jingwei, Zhao, Lei, Zhao, Ling, Zhao, M G, Zhao, Q, Zhao, S J, Zhao, T C, Zhao, X H, Zhao, Y B, Zhao, Z G, Zhao, A, Zhemchugov, B, Zheng, J P, Zheng, Y H, Zheng, Z P, Zheng, B, Zhong, J, Zhong, L, Zhou, Z L, Zhou, C, Zhu, K, Zhu, K J, Zhu, Q M, Zhu, X W, Zhu, Y S, Zhu, Z A, Zhu, J, Zhuang, B S, Zou, J H, Zou, J X, Zuo, and P, Zweber
Abstract: We present measurements of the charmonium state h(c)(1P(1)) made with 106x10(6) psi' events collected by BESIII at BEPCII. Clear signals are observed for psi'--pi0 h(c) with and without the subsequent radiative decay h(c)--gamma eta(c). First measurements of the absolute branching ratios B(psi'--pi0 h(c)) = (8.4+/-1.3+/-1.0) x 10(-4) and B(h(c)--gamma eta(c)) = (54.3+/-6.7+/-5.2)% are presented. A statistics-limited determination of the previously unmeasured h(c) width leads to an upper limit Gamma(h(c))1.44 MeV (90% confidence). Measurements of M(h(c)) = 3525.40+/-0.13+/-0.18 MeV/c2 and B(psi'--pi0 h(c)) x B(h(c)--gamma eta(c)) = (4.58+/-0.40+/-0.50) x 10(-4) are consistent with previous results.
Published: 2010

20. Evidence for ψ′ Decays into γπ0 and γη

Author: M, Ablikim, M N, Achasov, L, An, Q, An, Z H, An, J Z, Bai, R, Baldini, Y, Ban, J, Becker, N, Berger, M, Bertani, J M, Bian, I, Boyko, R A, Briere, V, Bytev, X, Cai, G F, Cao, X X, Cao, J F, Chang, G, Chelkov, G, Chen, H S, Chen, J C, Chen, M L, Chen, S J, Chen, Y, Chen, Y B, Chen, H P, Cheng, Y P, Chu, D, Cronin-Hennessy, H L, Dai, J P, Dai, D, Dedovich, Z Y, Deng, I, Denysenko, M, Destefanis, Y, Ding, L Y, Dong, M Y, Dong, S X, Du, M Y, Duan, R R, Fan, J, Fang, S S, Fang, F, Feldbauer, C Q, Feng, C D, Fu, J L, Fu, Y, Gao, C, Geng, K, Goetzen, W X, Gong, M, Greco, S, Grishin, M H, Gu, Y T, Gu, Y H, Guan, A Q, Guo, L B, Guo, Y P, Guo, X Q, Hao, F A, Harris, K L, He, M, He, Z Y, He, Y K, Heng, Z L, Hou, H M, Hu, J F, Hu, T, Hu, B, Huang, G M, Huang, J S, Huang, X T, Huang, Y P, Huang, T, Hussain, C S, Ji, Q, Ji, X B, Ji, X L, Ji, L K, Jia, L L, Jiang, X S, Jiang, J B, Jiao, Z, Jiao, D P, Jin, S, Jin, F F, Jing, M, Kavatsyuk, S, Komamiya, W, Kuehn, J S, Lange, J K C, Leung, Cheng, Li, Cui, Li, D M, Li, F, Li, G, Li, H B, Li, J C, Li, Lei, Li, N B, Li, Q J, Li, W D, Li, W G, Li, X L, Li, X N, Li, X Q, Li, X R, Li, Z B, Li, H, Liang, Y F, Liang, Y T, Liang, G R, Liao, X T, Liao, B J, Liu, C L, Liu, C X, Liu, C Y, Liu, F H, Liu, Fang, Liu, Feng, Liu, G C, Liu, H, Liu, H B, Liu, H M, Liu, H W, Liu, J P, Liu, K, Liu, K Y, Liu, Q, Liu, S B, Liu, X H, Liu, Y B, Liu, Y W, Liu, Yong, Liu, Z A, Liu, Z Q, Liu, H, Loehner, G R, Lu, H J, Lu, J G, Lu, Q W, Lu, X R, Lu, Y P, Lu, C L, Luo, M X, Luo, T, Luo, X L, Luo, C L, Ma, F C, Ma, H L, Ma, Q M, Ma, T, Ma, X, Ma, X Y, Ma, M, Maggiora, Q A, Malik, H, Mao, Y J, Mao, Z P, Mao, J G, Messchendorp, J, Min, R E, Mitchell, X H, Mo, C, Motzko, N Yu, Muchnoi, Y, Nefedov, Z, Ning, S L, Olsen, Q, Ouyang, S, Pacetti, M, Pelizaeus, K, Peters, J L, Ping, R G, Ping, R, Poling, C S J, Pun, M, Qi, S, Qian, C F, Qiao, X S, Qin, J F, Qiu, K H, Rashid, G, Rong, X D, Ruan, A, Sarantsev, J, Schulze, M, Shao, C P, Shen, X Y, Shen, H Y, Sheng, M R, Shepherd, X Y, Song, S, Sonoda, S, Spataro, B, Spruck, D H, Sun, G X, Sun, J F, Sun, S S, Sun, X D, Sun, Y J, Sun, Y Z, Sun, Z J, Sun, Z T, Sun, C J, Tang, X, Tang, X F, Tang, H L, Tian, D, Toth, G S, Varner, X, Wan, B Q, Wang, K, Wang, L L, Wang, L S, Wang, P, Wang, P L, Wang, Q, Wang, S G, Wang, X L, Wang, Y D, Wang, Y F, Wang, Y Q, Wang, Z, Wang, Z G, Wang, Z Y, Wang, D H, Wei, S P, Wen, U, Wiedner, L H, Wu, N, Wu, W, Wu, Z, Wu, Z J, Xiao, Y G, Xie, G F, Xu, G M, Xu, H, Xu, Y, Xu, Z R, Xu, Z Z, Xu, Z, Xue, L, Yan, W B, Yan, Y H, Yan, H X, Yang, M, Yang, T, Yang, Y, Yang, Y X, Yang, M, Ye, M H, Ye, B X, Yu, C X, Yu, L, Yu, C Z, Yuan, W L, Yuan, Y, Yuan, A A, Zafar, A, Zallo, Y, Zeng, B X, Zhang, B Y, Zhang, C C, Zhang, D H, Zhang, H H, Zhang, H Y, Zhang, J, Zhang, J W, Zhang, J Y, Zhang, J Z, Zhang, L, Zhang, S H, Zhang, T R, Zhang, X J, Zhang, X Y, Zhang, Y, Zhang, Y H, Zhang, Z P, Zhang, Z Y, Zhang, G, Zhao, H S, Zhao, Jiawei, Zhao, Jingwei, Zhao, Lei, Zhao, Ling, Zhao, M G, Zhao, Q, Zhao, S J, Zhao, T C, Zhao, X H, Zhao, Y B, Zhao, Z G, Zhao, Z L, Zhao, A, Zhemchugov, B, Zheng, J P, Zheng, Y H, Zheng, Z P, Zheng, B, Zhong, J, Zhong, L, Zhong, L, Zhou, X K, Zhou, X R, Zhou, C, Zhu, K, Zhu, K J, Zhu, S H, Zhu, X L, Zhu, X W, Zhu, Y S, Zhu, Z A, Zhu, J, Zhuang, B S, Zou, J H, Zou, J X, Zuo, and P, Zweber
Abstract: The decays ψ'→γπ(0), γη and γη' are studied using data collected with the BESIII detector at the BEPCII e(+)e(-) collider. The processes ψ'→γπ(0) and ψ'→γη are observed for the first time with signal significances of 4.6σ and 4.3σ, respectively. The branching fractions are determined to be B(ψ'→γπ(0))=(1.58±0.40±0.13)×10(-6), B(ψ'→γη)=(1.38±0.48±0.09)×10(-6), and B(ψ'→γη')=(126±3±8)×10(-6), where the first errors are statistical and the second ones systematic.
Published: 2010

21. Circumstellar Materials of SN 1987A

Author: C. S. J. Pun, Stefan Immler, and Kurt Weiler
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Supernova, Hubble space telescope, Astrophysics::Solar and Stellar Astrophysics, Electron temperature, Astrophysics::Earth and Planetary Astrophysics, Emission spectrum, Astrophysics::Galaxy Astrophysics, Space Telescope Imaging Spectrograph, FOIL method
Abstract: The geometric and physical properties of the circumstellar materials of SN 1987A were studied. The detailed structure of the SN 1987A equatorial inner ring (EIR) was investigated using two dimensional spectral images of the ring obtained on 1997 December 9 (day 3942) with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Space Telescope (HST). The data provided a valuable snapshot of the ring before foil fledge interaction with the supernova debris started. Geometric parameters of the EIR were determined for neutral and low‐ionization emission line species of H, He, O, N, S, and Ne. We also investigated the electron temperature, density, and elemental abundances around the EIR and we found no azimuthal variation around the ring.
Published: 2007
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22. Search for periodicities in theB8solar neutrino flux measured by the Sudbury Neutrino Observatory

Author: B. Aharmim, S. N. Ahmed, A. E. Anthony, E. W. Beier, A. Bellerive, M. Bergevin, S. D. Biller, M. G. Boulay, M. G. Bowler, Y. D. Chan, M. Chen, X. Chen, B. T. Cleveland, T. Costin, G. A. Cox, C. A. Currat, X. Dai, H. Deng, J. Detwiler, P. J. Doe, R. S. Dosanjh, G. Doucas, C. A. Duba, F. A. Duncan, M. Dunford, J. A. Dunmore, E. D. Earle, S. R. Elliott, H. C. Evans, G. T. Ewan, J. Farine, H. Fergani, F. Fleurot, J. A. Formaggio, W. Frati, B. G. Fulsom, N. Gagnon, J. TM. Goon, K. Graham, R. L. Hahn, A. L. Hallin, E. D. Hallman, W. B. Handler, C. K. Hargrove, P. J. Harvey, R. Hazama, K. M. Heeger, L. Heelan, W. J. Heintzelman, J. Heise, R. L. Helmer, R. J. Hemingway, A. Hime, M. A. Howe, M. Huang, E. Inrig, P. Jagam, N. A. Jelley, J. R. Klein, L. L. Kormos, M. S. Kos, A. Krüger, C. Kraus, C. B. Krauss, A. V. Krumins, T. Kutter, C. C. M. Kyba, H. Labranche, R. Lange, J. Law, I. T. Lawson, K. T. Lesko, J. R. Leslie, I. Levine, J. C. Loach, S. Luoma, R. MacLellan, S. Majerus, J. Maneira, A. D. Marino, N. McCauley, A. B. McDonald, S. McGee, C. Mifflin, K. K. S. Miknaitis, B. G. Nickel, A. J. Noble, E. B. Norman, N. S. Oblath, C. E. Okada, H. M. O’Keeffe, R. W. Ollerhead, G. D. Orebi Gann, J. L. Orrell, S. M. Oser, T. Ouvarova, S. J. M. Peeters, A. W. P. Poon, C. S. J. Pun, K. Rielage, B. C. Robertson, R. G. H. Robertson, E. Rollin, S. S. E. Rosendahl, M. H. Schwendener, S. R. Seibert, O. Simard, J. J. Simpson, C. J. Sims, D. Sinclair, L. Sinclair, P. Skensved, M. W. E. Smith, R. G. Stokstad, L. C. Stonehill, R. Tafirout, Y. Takeuchi, G. Tešić, M. Thomson, K. V. Tsang, T. Tsui, R. Van Berg, C. J. Virtue, B. L. Wall, D. Waller, C. E. Waltham, H. Wan Chan Tseung, D. L. Wark, J. Wendland, N. West, J. F. Wilkerson, J. R. Wilson, J. M. Wouters, M. Yeh, and K. Zuber
Subjects: Physics, Nuclear and High Energy Physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Solar neutrino, Flux, Astrophysics, Solar neutrino problem, 01 natural sciences, Radiation flux, Neutrino detector, 0103 physical sciences, High Energy Physics::Experiment, Neutrino, 010306 general physics, Lepton
Abstract: A search has been made for sinusoidal periodic variations in the 8B solar neutrino flux using data collected by the Sudbury Neutrino Observatory over a 4-year time interval. The variation at a period of 1 yr is consistent with modulation of the 8B neutrino flux by the Earth's orbital eccentricity. No significant sinusoidal periodicities are found with periods between 1 d and 10 years with either an unbinned maximum likelihood analysis or a Lomb-Scargle periodogram analysis. The data are inconsistent with the hypothesis that the results of the recent analysis by Sturrock et al., based on elastic scattering events in Super-Kamiokande, can be attributed to a 7% sinusoidal modulation of the total 8B neutrino flux.
Published: 2005
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23. Possible TeV Source Candidates In The Unidentified EGRET Sources

Author: Wei Wang, K. S. Cheng, C. S. J. Pun, and Z. J. Jiang
Subjects: Physics, COSMIC cancer database, Proper motion, biology, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Compton scattering, Magnetosphere, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galactic plane, biology.organism_classification, Galaxy, Pulsar, Space and Planetary Science, Egret, Astrophysics::Galaxy Astrophysics
Abstract: We study the $\gamma$-ray emission from the pulsar magnetosphere based on outer gap models, and the TeV radiation from pulsar wind nebulae (PWNe) through inverse Compton scattering using a one-zone model. We showed previously that GeV radiation from the magnetosphere of mature pulsars with ages of $\sim 10^5-10^6$ years old can contribute to the high latitude unidentified EGRET sources. We carry out Monte Carlo simulations of $\gamma$-ray pulsars in the Galaxy and the Gould Belt, assuming the pulsar birth rate, initial position, proper motion velocity, period, and magnetic field distribution and evolution based on observational statistics. We select from the simulation a sample of mature pulsars in the Galactic plane ($|b|\leq 5^\circ$) and in the high latitude ($|b|> 5^\circ$) which could be detected by EGRET. The TeV flux from the pulsar wind nebulae of our simulated sample through the inverse Compton scattering by relativistic electrons on the microwave cosmic background and synchrotron seed photons are calculated. The predicted fluxes are consistent with the present observational constraints. We suggest that strong EGRET sources can be potential TeV source candidates for present and future ground-based TeV telescopes., Comment: Minor changes, MNRAS in press
Published: 2004

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23 results on '"C. S. J. Pun"'

1. Charged-current non-standard neutrino interactions at Daya Bay

2. Extraction of the ^{235}U and ^{239}Pu Antineutrino Spectra at Daya Bay

3. Publisher’s Note: Measurement of cosmic-ray muons and muon-induced neutrons in the Aberdeen Tunnel Underground Laboratory [Phys. Rev. D 93 , 072005 (2016)]

4. Study of $J/ψ\to p\bar{p}$ and $J/ψ\to n\bar{n}$

5. Two-photon widths of the $χ_{c0, 2}$ states and helicity analysis for $χ_{c2}\arγγ$}

6. Could electron-positron annihilation lines in the Galactic center result from pulsar winds?

7. The Axisymmetric Ejecta of Supernova 1987A

8. 56Ni Mixing in the Outer Layers of SN 1987A

9. Analysis of Type IIn SN 1998S: Effects of Circumstellar Interaction on Observed Spectra

10. [ITAL]Hubble Space Telescope[/ITAL] Spectroscopy of Spot 1 on the Circumstellar Ring of SN 1987A

11. High-Velocity L[CLC]y[/CLC]α Emission from SNR 1987A

12. Observation of two new N* resonances in the decay ψ(3686)→ppπ0

13. Evidence for the direct two-photon transition from ψ(3686) to J/ψ

14. ηπ+ π- resonant structure around 1.8 GeV/c(2) and η(1405) in J/ψ → ωηπ+ π

15. Observation of χ(c1) decays into vector meson pairs φφ, ωω, and ωφ

16. Confirmation of the X(1835) and Observation of the Resonances X(2120) and X(2370) in J/ψ→γπ+π-η′

17. X-ray illumination of the ejecta of supernova 1987A

18. Evidence forψ′Decays intoγπ0andγη

19. Measurements of h(c)(1P(1)) in psi' decays

20. Evidence for ψ′ Decays into γπ0 and γη

21. Circumstellar Materials of SN 1987A

22. Search for periodicities in theB8solar neutrino flux measured by the Sudbury Neutrino Observatory

23. Possible TeV Source Candidates In The Unidentified EGRET Sources

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23 results on '"C. S. J. Pun"'

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