科学通报(英文版)2024，Vol.69Issue(18) ：2833-2841.DOI:10.1016/j.scib.2024.07.017

Evidence for particle acceleration approaching PeV energies in the W51 complex

LHAASO Collaboration Zhen Cao F.Aharonian Axikegu Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi W.Bian A.V.Bukevich Q.Cao W.Y.Cao Zhe Cao J.Chang J.F.Chang A.M.Chen E.S.Chen H.X.Chen Liang Chen Lin Chen Long Chen M.J.Chen M.L.Chen Q.H.Chen S.Chen S.H.Chen S.Z.Chen T.L.Chen Y.Chen N.Cheng Y.D.Cheng M.Y.Cui S.W.Cui X.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu X.Q.Dong K.K.Duan J.H.Fan Y.Z.Fan J.Fang J.H.Fang K.Fang C.F.Feng H.Feng L.Feng S.H.Feng X.T.Feng Y.Feng Y.L.Feng S.Gabici B.Gao C.D.Gao Q.Gao W.Gao W.K.Gao M.M.Ge L.S.Geng G.Giacinti G.H.Gong Q.B.Gou M.H.Gu F.L.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han M.Hasan H.H.He H.N.He J.Y.He Y.He Y.K.Hor B.W.Hou C.Hou X.Hou H.B.Hu Q.Hu S.C.Hu D.H.Huang T.Q.Huang W.J.Huang X.T.Huang X.Y.Huang Y.Huang X.L.Ji H.Y.Jia K.Jia K.Jiang X.W.Jiang Z.J.Jiang M.Jin M.M.Kang I.Karpikov D.Kuleshov K.Kurinov B.B.Li C.M.Li Cheng Li Cong Li D.Li F.Li H.B.Li H.C.Li Jian Li Jie Li K.Li S.D.Li W.L.Li X.R.Li Xin Li Y.Z.Li Zhe Li Zhuo Li E.W.Liang Y.F.Liang S.J.Lin B.Liu C.Liu D.Liu D.B.Liu H.Liu H.D.Liu J.Liu J.L.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.Liu Y.N.Liu Q.Luo Y.Luo H.K.Lv B.Q.Ma L.L.Ma X.H.Ma J.R.Mao Z.Min W.Mitthumsiri H.J.Mu Y.C.Nan A.Neronov L.J.Ou P.Pattarakijwanich Z.Y.Pei J.C.Qi M.Y.Qi B.Q.Qiao J.J.Qin A.Raza D.Ruffolo A.Sáiz M.Saeed D.Semikoz L.Shao O.Shchegolev X.D.Sheng F.W.Shu H.C.Song Yu.V.Stenkin V.Stepanov Y.Su D.X.Sun Q.N.Sun X.N.Sun Z.B.Sun J.Takata P.H.T.Tam Q.W.Tang R.Tang Z.B.Tang W.W.Tian C.Wang C.B.Wang G.W.Wang H.G.Wang H.H.Wang J.C.Wang Kai Wang L.P.Wang L.Y.Wang P.H.Wang R Wang W.Wang X.G.Wang X.Y.Wang Y.Wang Y.D.Wang Y.J.Wang Z.H.Wang Z.X.Wang Zhen Wang Zheng Wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.Wu H.R.Wu Q.W.Wu S.Wu X.F.Wu Y.S.Wu S.Q.Xi J.Xia G.M.Xiang D.X.Xiao G.Xiao Y.L.Xin Y.Xing D.R.Xiong Z.Xiong D.L.Xu R F.Xu R.X.Xu W.L.Xu L Xue D.H.Yan J.Z.Yan T.Yan C.W.Yang C.Y.Yang F.Yang F.F.Yang L.L.Yang M.J.Yang R.Z.Yang W.X.Yang Y.H.Yao Z.G.Yao L.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.Yue H.D.Zeng T.X.Zeng W.Zeng M.Zha B.B.Zhang F.Zhang H.Zhang H.M.Zhang H.Y.Zhang J.L.Zhang Li Zhang P.F.Zhang P.P.Zhang R.Zhang S.B.Zhang S.R.Zhang S.S.Zhang X.Zhang X.P.Zhang Y.F.Zhang Yi Zhang Yong Zhang B.Zhao J.Zhao L Zhao LZ.Zhao S.P.Zhao X.H.Zhao F.Zheng W.J.Zhong B.Zhou H.Zhou J.N.Zhou M.Zhou P.Zhou R.Zhou X.X.Zhou B.Y.Zhu C.G.Zhu F.R.Zhu H.Zhu K.J.Zhu Y.C.Zou X.Zuo S.Celli
科学通报(英文版)2024，Vol.69Issue(18) ：2833-2841.DOI:10.1016/j.scib.2024.07.017
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  • NETL
  • NSTL
  • 万方数据

Evidence for particle acceleration approaching PeV energies in the W51 complex

LHAASO Collaboration Zhen Cao 1F.Aharonian 2Axikegu 3Y.X.Bai 4Y.W.Bao 5D.Bastieri 6X.J.Bi 1Y.J.Bi 4W.Bian 7A.V.Bukevich 8Q.Cao 9W.Y.Cao 10Zhe Cao 11J.Chang 12J.F.Chang 13A.M.Chen 7E.S.Chen 1H.X.Chen 14Liang Chen 15Lin Chen 3Long Chen 3M.J.Chen 4M.L.Chen 13Q.H.Chen 3S.Chen 16S.H.Chen 1S.Z.Chen 4T.L.Chen 17Y.Chen 5N.Cheng 4Y.D.Cheng 1M.Y.Cui 12S.W.Cui 9X.H.Cui 18Y.D.Cui 19B.Z.Dai 16H.L.Dai 13Z.G.Dai 10Danzengluobu 17X.Q.Dong 1K.K.Duan 12J.H.Fan 6Y.Z.Fan 12J.Fang 16J.H.Fang 14K.Fang 4C.F.Feng 20H.Feng 21L.Feng 12S.H.Feng 4X.T.Feng 20Y.Feng 14Y.L.Feng 17S.Gabici 22B.Gao 4C.D.Gao 20Q.Gao 17W.Gao 4W.K.Gao 1M.M.Ge 16L.S.Geng 4G.Giacinti 7G.H.Gong 23Q.B.Gou 4M.H.Gu 13F.L.Guo 15X.L.Guo 3Y.Q.Guo 4Y.Y.Guo 12Y.A.Han 24M.Hasan 1H.H.He 1H.N.He 12J.Y.He 12Y.He 3Y.K.Hor 19B.W.Hou 1C.Hou 4X.Hou 25H.B.Hu 1Q.Hu 26S.C.Hu 27D.H.Huang 3T.Q.Huang 4W.J.Huang 19X.T.Huang 20X.Y.Huang 12Y.Huang 1X.L.Ji 13H.Y.Jia 3K.Jia 20K.Jiang 11X.W.Jiang 4Z.J.Jiang 16M.Jin 3M.M.Kang 28I.Karpikov 8D.Kuleshov 8K.Kurinov 8B.B.Li 9C.M.Li 5Cheng Li 11Cong Li 4D.Li 1F.Li 13H.B.Li 4H.C.Li 4Jian Li 10Jie Li 13K.Li 4S.D.Li 29W.L.Li 20X.R.Li 4Xin Li 11Y.Z.Li 1Zhe Li 4Zhuo Li 30E.W.Liang 31Y.F.Liang 31S.J.Lin 19B.Liu 10C.Liu 4D.Liu 20D.B.Liu 7H.Liu 3H.D.Liu 24J.Liu 4J.L.Liu 4M.Y.Liu 17R.Y.Liu 5S.M.Liu 3W.Liu 4Y.Liu 6Y.N.Liu 23Q.Luo 19Y.Luo 7H.K.Lv 4B.Q.Ma 30L.L.Ma 4X.H.Ma 4J.R.Mao 25Z.Min 4W.Mitthumsiri 32H.J.Mu 24Y.C.Nan 4A.Neronov 22L.J.Ou 6P.Pattarakijwanich 32Z.Y.Pei 6J.C.Qi 1M.Y.Qi 4B.Q.Qiao 4J.J.Qin 10A.Raza 1D.Ruffolo 32A.Sáiz 32M.Saeed 1D.Semikoz 22L.Shao 9O.Shchegolev 33X.D.Sheng 4F.W.Shu 34H.C.Song 30Yu.V.Stenkin 33V.Stepanov 8Y.Su 12D.X.Sun 26Q.N.Sun 3X.N.Sun 31Z.B.Sun 35J.Takata 36P.H.T.Tam 19Q.W.Tang 34R.Tang 7Z.B.Tang 11W.W.Tian 37C.Wang 35C.B.Wang 3G.W.Wang 10H.G.Wang 6H.H.Wang 19J.C.Wang 25Kai Wang 5L.P.Wang 1L.Y.Wang 4P.H.Wang 3R Wang 20W.Wang 19X.G.Wang 31X.Y.Wang 5Y.Wang 3Y.D.Wang 4Y.J.Wang 4Z.H.Wang 28Z.X.Wang 16Zhen Wang 7Zheng Wang 13D.M.Wei 12J.J.Wei 12Y.J.Wei 1T.Wen 16C.Y.Wu 4H.R.Wu 4Q.W.Wu 36S.Wu 4X.F.Wu 12Y.S.Wu 10S.Q.Xi 4J.Xia 26G.M.Xiang 29D.X.Xiao 9G.Xiao 4Y.L.Xin 3Y.Xing 15D.R.Xiong 25Z.Xiong 1D.L.Xu 7R F.Xu 1R.X.Xu 30W.L.Xu 28L Xue 20D.H.Yan 16J.Z.Yan 12T.Yan 4C.W.Yang 28C.Y.Yang 25F.Yang 9F.F.Yang 13L.L.Yang 19M.J.Yang 4R.Z.Yang 10W.X.Yang 6Y.H.Yao 4Z.G.Yao 4L.Q.Yin 4N.Yin 20X.H.You 4Z.Y.You 4Y.H.Yu 10Q.Yuan 12H.Yue 1H.D.Zeng 12T.X.Zeng 13W.Zeng 16M.Zha 4B.B.Zhang 5F.Zhang 3H.Zhang 7H.M.Zhang 5H.Y.Zhang 4J.L.Zhang 18Li Zhang 16P.F.Zhang 16P.P.Zhang 26R.Zhang 26S.B.Zhang 37S.R.Zhang 9S.S.Zhang 4X.Zhang 5X.P.Zhang 4Y.F.Zhang 3Yi Zhang 38Yong Zhang 4B.Zhao 3J.Zhao 4L Zhao 11LZ.Zhao 9S.P.Zhao 12X.H.Zhao 25F.Zheng 35W.J.Zhong 5B.Zhou 4H.Zhou 7J.N.Zhou 15M.Zhou 34P.Zhou 5R.Zhou 28X.X.Zhou 1B.Y.Zhu 26C.G.Zhu 20F.R.Zhu 3H.Zhu 18K.J.Zhu 39Y.C.Zou 36X.Zuo 4S.Celli40
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作者信息

  • 1. Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center,Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049,China;University of Chinese Academy of Sciences,Beijing 100049,China;TIANFU Cosmic Ray Research Center,Chengdu,China
  • 2. Dublin Institute for Advanced Studies,31 Fitzwilliam Place,2 Dublin,Ireland;Max-Planck-Institut for Nuclear Physics,P.O.Box 103980,Hei-delberg 69029,Germany
  • 3. School of Physical Science and Technology & School of Information Science and Technology,Southwest Jiaotong University,Chengdu 610031,China
  • 4. Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center,Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049,China;TIANFU Cosmic Ray Research Center,Chengdu,China
  • 5. School of Astronomy and Space Science,Nanjing University Nanjing 210023,China
  • 6. Center for Astrophysics,Guangzhou University,Guangzhou 510006,China
  • 7. Tsung-Dao Lee Institute&School of Physics and Astronomy,Shanghai Jiao Tong University,Shanghai 200240,China
  • 8. Institute for Nuclear Research of Russian Academy of Sciences,Moscow 117312,Russia
  • 9. Hebei Normal University,Shijiazhuang 050024,China
  • 10. University of Science and Technology of China,Hefei,230026,China
  • 11. State Key Laboratory of Particle Detection and Electronics,China;University of Science and Technology of China,Hefei 230026,China
  • 12. Key Laboratory of Dark Matter and Space Astronomy & Key Laboratory of Radio Astronomy,Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210023,China
  • 13. Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center,Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049,China;TIANFU Cosmic Ray Research Center,Chengdu,China;State Key Laboratory of Particle Detection and Electronics,China
  • 14. Research Center for Astronomical Computing,Zhejiang Laboratory,Hangzhou 311121,China
  • 15. Key Laboratory for Research in Galaxies and Cosmology,Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China
  • 16. School of Physics and Astronomy,Yunnan University,Kunming 650091,China
  • 17. Key Laboratory of Cosmic Rays(Tibet University),Ministry of Education,Lhasa 850000,China
  • 18. National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China
  • 19. School of Physics and Astronomy(Zhuhai)& School of Physics(Guangzhou)& Sino-French Institute of Nuclear Engineering and Technology(Zhuhai),Sun Yat-sen University,Zhuhai 519000 &Guangzhou 510275,Guangdong,China
  • 20. Institute of Frontier and Interdisciplinary Science,Shandong University,Qingdao 266237,China
  • 21. Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center,Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049,China
  • 22. APC,Université Paris Cité,CNRS/IN2P3,CEA/IRFU,Observatoire de Paris,Paris 119 75205,France
  • 23. Department of Engineering Physics,Tsinghua University,Beijing 100084,China
  • 24. School of Physics and Microelectronics,Zhengzhou University,Zhengzhou 450001,China
  • 25. Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China
  • 26. University of Science and Technology of China,Hefei 230026,China;Key Laboratory of Dark Matter and Space Astronomy & Key Laboratory of Radio Astronomy,Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210023,China
  • 27. Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center,Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049,China;TIANFU Cosmic Ray Research Center,Chengdu,China;China Center of Advanced Science and Technology,Beijing 100190,China
  • 28. College of Physics,Sichuan University,Chengdu 610065,China
  • 29. Key Laboratory for Research in Galaxies and Cosmology,Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China;University of Chinese Academy of Sciences,Beijing 100049,China
  • 30. School of Physics,Peking University,Beijing 100871,China
  • 31. Guangxi Key Laboratory for Relativistic Astrophysics,School of Physical Science and Technology,Guangxi University,Nanning 530004,China
  • 32. Department of Physics,Faculty of Science,Mahidol University,Bangkok 10400,Thailand
  • 33. Institute for Nuclear Research of Russian Academy of Sciences,Moscow 117312,Russia;Moscow Institute of Physics and Technology,Moscow 141700,Russia
  • 34. Center for Relativistic Astrophysics and High Energy Physics,School of Physics and Materials Science & Institute of Space Science and Technology,Nanchang University,Nanchang 330031,China
  • 35. National Space Science Center,Chinese Academy of Sciences,Beijing 100190,China
  • 36. School of Physics,Huazhong University of Science and Technology,Wuhan,430074,China
  • 37. University of Chinese Academy of Sciences,Beijing 100049,China;National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China
  • 38. Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center,Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049,China;Key Laboratory of Dark Matter and Space Astronomy & Key Laboratory of Radio Astronomy,Purple Mountain Observatory,Chi-nese Academy of Sciences,Nanjing 210023,China
  • 39. Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center,Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049,China;University of Chinese Academy of Sciences,Beijing 100049,China;TIANFU Cosmic Ray Research Center,Chengdu,China;State Key Laboratory of Particle Detection and Electronics,China
  • 40. Department of Physics,Sapienza University of Rome,Piazzale Aldo Moro 2,Rome 00185,Italy
  • 折叠

Abstract

The γ-ray emission from the W51 complex is widely acknowledged to be attributed to the interaction between the cosmic rays(CRs)accelerated by the shock of supernova remnant(SNR)W51C and the dense molecular clouds in the adjacent star-forming region,W51B.However,the maximum acceleration capa-bility of W51C for CRs remains elusive.Based on observations conducted with the Large High Altitude Air Shower Observatory(LHAASO),we report a significant detection of γ rays emanating from the W51 com-plex,with energies from 2 to 200 TeV.The LHAASO measurements,for the first time,extend the y-ray emission from the W51 complex beyond 100 TeV and reveal a significant spectrum bending at tens of TeV.By combining the"π0-decay bump"featured data from Fermi-LAT,the broadband y-ray spectrum of the W51 region can be well-characterized by a simple pp-collision model.The observed spectral bend-ing feature suggests an exponential cutoff at～400 TeV or a power-law break at～200 TeV in the CR pro-ton spectrum,most likely providing the first evidence of SNRs serving as CR accelerators approaching the PeV regime.Additionally,two young star clusters within W51B could also be theoretically viable to pro-duce the most energetic γ rays observed by LHAASO.Our findings strongly support the presence of extreme CR accelerators within the W51 complex and provide new insights into the origin of Galactic CRs.

Key words

UHE γ-ray/Cosmic rays/SNRW51C/Star clusters

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基金项目

National Natural Science Foundation of China(12393851)

National Natural Science Foundation of China(12261160362)

National Natural Science Foundation of China(12393852)

National Natural Science Foundation of China(12393853)

National Natural Science Foundation of China(12393854)

National Natural Science Foundation of China(12022502)

National Natural Science Foundation of China(2205314)

National Natural Science Foundation of China(12105301)

National Natural Science Foundation of China(12105292)

National Natural Science Foundation of China(12105294)

National Natural Science Foundation of China(12005246)

Department of Science and Technology of Sichuan Province(24NSFJQ0060)

Department of Science and Technology of Sichuan Province(2024NSFSC0449)

Project for Young Scientists in Basic Research of Chinese Academy of Sciences(YSBR-061)

Project for Young Scientists in Basic Research of Chinese Academy of Sciences(2022010)

in Thailand by the National Science and Technology Development Agency(NSTDA)()

National Research Council of Thailand(NRCT):High-Potential Research Team Grant Program(N42A650868)

Chengdu Management Committee of Tianfu New Area()

Milky Way Imaging Scroll Painting(MWISP)project()

National Key R&D Program of China(2023YFA1608000)

National Key R&D Program of China(2017YFA0402701)

CAS Key Research Program of Frontier Sciences(QYZDJ-SSW-SLH047)

出版年

2024
科学通报(英文版)
中国科学院

科学通报(英文版)

CSTPCD
ISSN：1001-6538
参考文献量1
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