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Reconstruction of Cherenkov image bymultiple telescopes of LHAASO-WFCTA

Radiation Detection Technology and Methods 2022年第4期6卷 544-557页

作者： F.Aharonian Q.An Axikegu L.X.Bai Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi J.T.Cai zhe Cao zhen Cao J.Chang J.F.Chang E.S.Chen Liang Chen Liang Chen Long Chen M.J.Chen M.L.Chen Q.H.Chen S.H.Chen S.z.Chen T.L.Chen Y.Chen H.L.Cheng N.Cheng Y.D.Cheng S.W.Cui X.H.Cui Y.D.Cui B.D’Ettorre Piazzoli B.z.Dai H.L.Dai z.G.Dai Danzengluobu Ddella Volpe K.K.Duan J.H.Fan Y.z.Fan z.X.Fan J.Fang K.Fang C.F.Feng L.Feng S.H.Feng X.T.Feng Y.L.Feng B.Gao C.D.Gao L.Q.Gao Q.Gao W.Gao W.K.Gao M.M.Ge L.S.Geng G.H.Gong Q.B.Gou M.H.Gu F.L.Guo J.G.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He S.L.He X.B.He Y.He M.Heller Y.K.Hor C.Hou X.Hou H.B.Hu Q.Hu S.Hu S.C.Hu X.J.Hu D.H.Huang W.H.Huang X.T.Huang X.Y.Huang Y.Huang z.C.Huang X.L.Ji H.Y.Jia K.Jia K.Jiang z.J.Jiang M.Jin M.M.Kang T.Ke D.Kuleshov K.Levochkin B.B.Li Cheng Li Cong Li F.Li H.B.Li H.C.Li H.Y.Li J.Li Jian Li Jie Li K.Li WLLi XRLi Xin Li Xin Li YzLi zhe Li zhuo Li E.W.Liang Y.F.Liang S.J.Lin B.Liu C.Liu D.Liu H.Liu H.D.Liu J.Liu J.L.Liu J.S.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.Liu Y.N.Liu W.J.Long R.Lu Q.Luo H.K.Lv B.Q.Ma L.L.Ma X.H.Ma J.R.Mao A.Masood z.min W.Mitthumsiri Y.C.Nan z.W.Ou B.Y.Pang P.Pattarakijwanich z.Y.Pei M.Y.Qi Y.Q.Qi B.Q.Qiao J.J.Qin D.Ruffolo A.Sáiz C.Y.Shao L.Shao O.Shchegolev X.D.Sheng J.Y.Shi H.C.Song Yu.V.Stenkin V.Stepanov Y.Su Q.N.Sun X.N.Sun z.B.Sun P.H.T.Tam z.B.Tang W.W.Tian B.D.Wang C.Wang H.Wang H.G.Wang J.C.Wang J.S.Wang L.P.Wang L.Y.Wang R.Wang R.N.Wang W.Wang X.G.Wang X.Y.Wang Y.Wang Y.D.Wang Y.J.Wang Y.P.Wang z.H.Wang z.X.Wang zhen Wang zheng Wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.Wu H.R.Wu S.Wu X.F.Wu Y.S.Wu S.Q.Xi J.Xia J.J.Xia G.M.Xiang D.X.Xiao G.Xiao G.G.Xin Y.L.Xin Y.Xing z.Xiong D.L.Xu R.X.Xu L.Xue D.H.Yan J.z.Yan C.W.Yang F.F.Yang H.W.Yang J.Y.Yang L.L.Yang M.J.Yang R.z.Yang S.B.Yang Y.H.Yao z.G.Yao Y.M.Ye 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 z.K.zeng M.zha X.X.zhai B.B.zhang F.zhang H.M.zhang H.Y.zhang J.L.zhang L.X.zhang Li zhang Lu zhang P.F.zhang P.P.zhang R.zhang S.B.zhang S.R.zhang S. Key Laboratory of Particle Astrophyics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2DublinIreland Max-Planck-Institut for Nuclear Physics P.O.Box 10398069029 HeidelbergGermany State Key Laboratory of Particle Detection and Electronics BeijingChina University of Science and Technology of China Hefei 230026AnhuiChina School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of Physics Sichuan UniversityChengdu 610065SichuanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China Hebei Normal University Shijiazhuang 050024HebeiChina School of Physics and Astronomy(zhuhai)&Sino-French Institute of Nuclear Engineering and Technology(zhuhai) Sun Yat-sen UniversityZhuhai 519000China School of Physics(Guangzhou) Sun Yat-sen UniversityGuangzhou 510275GuangdongChina Dipartimento di Fisica dell’Universitàdi Napoli“Federico II” Complesso Universitario di Monte Sant’Angelovia Cinthia80126 NapoliItaly School of Physics and Astronomy Yunnan UniversityKunming 650091YunnanChina Département de Physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde Genève

Introduction One of main scientiﬁc goals of the Large High Altitude Air Shower Observatory(LHAASO)is to accurately measure the energy spectra of different cosmic ray compositions around the‘knee’*** Wide Field-of-View(FoV)Cherenkov Telescope Array(WFCTA),which is one of the main detectors of LHAASO and has 18 telescopes,is built to achieve this *** telescopes are put together and point to connected directions for a larger *** Telescopes are deployed spatially as close as possible,but due to their own size,the distance between two adjacent telescopes is about 10 ***,the Cherenkov lateral distribution and the parallax between the two telescopes should be considered in the event building process for images crossing over the boundaries of FoVs of the *** event building method for Cherenkov images measured by multiple telescopes of WFCTA is *** performance of the shower measurements using the combined images is evaluated by comparing with showers that are fully contained by a virtual telescope in *** and conclusion It is proved that the developed event building process can help to increase the FoV of WFCTA by 30%while maintaining the same reconstruction quality,compared to the separate telescope reconstruction method.

关键词： method directions conclusion

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LHAASO-KM2A detector simulation using Geant4

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Radiation Detection Technology and Methods 2024年第3期8卷 1437-1447页

作者： zhen Cao F.Aharonian Q.An Axikegu Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi J.T.Cai Q.Cao W.Y.Cao zhe Cao J.Chang J.F.Chang A.M.Chen E.S.Chen Liang Chen Lin Chen Long Chen M.J.Chen M.L.Chen Q.H.Chen S.H.Chen S.z.Chen T.L.Chen Y.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 K.Fang C.F.Feng L.Feng S.H.Feng X.T.Feng Y.L.Feng S.Gabici B.Gao C.D.Gao L.Q.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 H.H.He H.N.He J.Y.He X.B.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 z.C.Huang X.L.Ji H.Y.Jia K.Jia K.Jiang X.W.Jiang z.J.Jiang M.Jin M.M.Kang T.Ke D.Kuleshov K.Kurinov B.B.Li Cheng Li Cong Li D.Li F.Li H.B.Li H.C.Li H.Y.Li J.Li Jian Li Jie Li K.Li W.L.Li 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 H.Liu H.D.Liu J.Liu J.L.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.Liu Y.N.Liu R.Lu Q.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 z.W.Ou B.Y.Pang P.Pattarakijwanich z.Y.Pei M.Y.Qi Y.Q.Qi B.Q.Qiao J.J.Qin D.Ruffolo A.Sáiz D.Semikoz C.Y.Shao L.Shao O.Shchegolev X.D.Sheng F.W.Shu H.C.Song Yu.V.Stenkin V.Stepanov Y.Su Q.N.Sun X.N.Sun z.B.Sun P.H.T.Tam Q.W.Tang z.B.Tang W.W.Tian C.Wang C.B.Wang G.W.Wang H.G.Wang H.H.Wang J.C.Wang K.Wang L.P.Wang L.Y.Wang P.H.Wang R.Wang W.Wang X.G.Wang X.Y.Wang Y.Wang Y.D.Wang Y.J.Wang z.H.Wang z.X.Wang zhen Wang zheng Wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.Wu H.R.Wu S.Wu X.F.Wu Y.S.Wu S.Q.Xi J.Xia J.J.Xia G.M.Xiang D.X.Xiao G.Xiao G.G.Xin Y.L.Xin Y.Xing 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 F.Yang F.F.Yang H.W.Yang J.Y.Yang L.L.Yang M.J.Yang R.z.Yang S.B.Yang Y.H.Yao z.G.Yao Y.M.Ye 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.M.zhang H.Y.zhang J.L.zhang L.X.zhang Li zhang P.F.zhang P.P.zhang R.zhang S.B.zh Key Laboratory of Particle Astrophysics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing100049China University of Chinese Academy of Sciences Beijing100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institute for Nuclear Physics 69029Heidelberg103980Germany State Key Laboratory of Particle Detection and Electronics BeijingChina University of Science and Technology of China Hefei230026AnhuiChina School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu610031SichuanChina School of Astronomy and Space Science Nanjing UniversityNanjing210023JiangsuChina Center for Astrophysics Guangzhou UniversityGuangzhou510006GuangdongChina Hebei Normal University Shijiazhuang050024HebeiChina Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Physics and Astronomy(zhuhai)&School of Physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(zhuhai) Sun Yat-sen UniversityGuangzhouZhuhai 510275519000GuangdongChina School of Physics and Astronomy Yunnan UniversityKunming 650091YunnanChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina APC UniversitéParis CitéCNRS/IN2P3CEA/IRFUObservatoire de ParisParis 11975205France Department of Engineering Phys

KM2A is one of the main sub-arrays of LHAASO,working on gamma ray astronomy and cosmic ray physics at energies above 10 *** simulation is the important foundation for estimating detector performance and data *** is a big challenge to simulate the KM2A detector in the framework of Geant4 due to the need to track numerous photons from a large number of detector units(>6000)with large altitude difference(30)and huge coverage(1.3).In this paper,the design of the KM2A simulation code G4KM2A based on Geant4 is *** process of G4KM2A is optimized mainly in memory consumption to avoid memory *** simplifications are used to significantly speed up the execution of *** running time is reduced by at least 30 times compared to full detector *** particle distributions and the core/angle resolution comparison between simulation and experimental data of the full KM2A array are also presented,which show good agreement.

关键词： LHAASO KM2A Simulation GEANT4

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Determination of strain-dependent soil water retention characteristics from gradation curve

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Journal of Rock Mechanics and Geotechnical Engineering 2020年第6期12卷 1356-1360页

作者： min Wang GNPande Stan Pietruszczak z.X.zeng zienkiewicz Centre for Computational Engineering Swansea UniversitySwanseaSA18ENUK Civil Engineering McMaster UniversityHamiltonOntarioL8S 4L8Canada École des Ponts ParisTech Champs-sur-MarneMarne-la-Vallée77455France

The importance of soil water retention characteristics in modelling the hydro-mechanical response of unsaturated soils has been well recognised by many investigators in recent *** of strain-dependent soil water retention curve(SWRC)is likely to be extraordinarily *** first two authors have recently shown that SWRC can be computed from the gradation curve and the calculation result is consistent with the experimental results obtained from pressure plate *** this paper,based on a hypothesis related to change in the pore size distribution(POSD)due to volumetric strain of soil skeleton,a method to compute strain-dependent SWRC is *** is found that at initial degrees of saturation higher than 0.8,the influence of volumetric strain may be marginal whilst at initial degrees of saturation lower than 0.8,its influence is likely to be *** all cases,the gradation curve of the soil affects the SWRC.

关键词： Soil water retention curve(SWRC) Gradation curve Pore size distribution(POSD) Unsaturated soil

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由超拍电子伏特加速器产生的超高能伽马射线气泡

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Science Bulletin 2024年第4期69卷 449-457页

作者： LHAASO Collaboration zhen Cao Chuandong Gao Cong Li Ruo-Yu Liu Ruizhi Yang 不详 Key Laboratory of Particle Astrophyics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China University of Science and Technology of China Hefei 230026China

We report the detection of aγ-ray bubble spanning at least 100deg2 in ultra-high energy(UHE)up to a few PeV in the direction of the star-forming region Cygnus X,implying the presence super PeVatron(s)accelerating protons to at least 10 PeV.A log-parabola form with the photon indexΓ(E)=(2.71±0.02)+(0.11±0.02)×log10(E/10 TeV)is found fitting the gamma-ray energy spectrum of the bubble *** sources,“hot spots”correlated with very massive molecular clouds,and a quasi-spherical amorphousγ-ray emitter with a sharp central brightening are observed in the *** the core of~0.5°,spatially associating with a region containing massive OB association(Cygnus OB2)and a microquasar(Cygnus X-3),as well as previously reported multi-TeV sources,an enhanced concentration of UHEγ-rays is observed with 2 photons at energies above 1 *** general feature of the bubble,the morphology,and the energy spectrum,are reasonably reproduced by the assumption of a particle accelerator in the core,continuously injecting protons into the ambient medium.

关键词： Cosmic rays γ-rays Interstellar medium Star cluster

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Evidence for particle acceleration approaching PeV energies in the W51 complex

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Science Bulletin 2024年第18期69卷 2833-2841页

作者： 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 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 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 不详 Key Laboratory of Particle Astrophysics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institut for Nuclear Physics P.O.Box 103980Heidelberg 69029Germany School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Institute for Nuclear Research of Russian Academy of Sciences Moscow 117312Russia Hebei Normal University Shijiazhuang 050024China University of Science and Technology of China Hefei 230026China State Key Laboratory of Particle Detection and Electronics China Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Research Center for Astronomical Computing Zhejiang LaboratoryHangzhou 311121China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China School of Physics and Astronomy Yunnan UniversityKunming 650091China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Physics and Astronomy(zhuhai)&School of Physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(zhuhai) Sun Yat-sen UniversityZhuhai 519000&Guangzhou 510275GuangdongChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China APC UniversitéParis Cité

Theγ-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,***,the maximum acceleration capability of W51C for CRs remains *** on observations conducted with the Large High Altitude Air Shower Observatory(LHAASO),we report a significant detection ofγrays emanating from the W51 complex,with energies from 2 to 200 *** LHAASO measurements,for the first time,extend theγ-ray emission from the W51 complex beyond 100 TeV and reveal a significant spectrum bending at tens of *** combining the"π^(0)-decay bump"featured data from Fermi-LAT,the broadbandγ-ray spectrum of the W51 region can be well-characterized by a simple pp-collision *** observed spectral bending feature suggests an exponential cutoff at~400 TeV or a power-law break at~200 TeV in the CR proton spectrum,most likely providing the first evidence of SNRs serving as CR accelerators approaching the PeV ***,two young star clusters within W51B could also be theoretically viable to produce the most energeticγrays observed by *** findings strongly support the presence of extreme CR accelerators within the W51 complex and provide new insights into the origin of Galactic CRs.

关键词： UHE c-ray Cosmic rays SNR W51C Star clusters

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踝关节骨折术后踝穴冠状位角度波动与关节功能恢复的关系

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中国组织工程研究 2025年第9期29卷 1820-1826页

作者：刘琰王铠吴敏泰州市中医院骨科江苏省泰州市225300

背景:踝关节骨折术后的踝穴形态指标会出现相应变化,而其中踝穴冠状位角度变化与踝关节的功能恢复之间存在一定的关联,既往研究大多探讨患者术后踝穴高度恢复,故研究踝关节骨折术后踝穴冠状位角度的波动与关节功能恢复的相关性具有一定... 详细信息

背景:踝关节骨折术后的踝穴形态指标会出现相应变化,而其中踝穴冠状位角度变化与踝关节的功能恢复之间存在一定的关联,既往研究大多探讨患者术后踝穴高度恢复,故研究踝关节骨折术后踝穴冠状位角度的波动与关节功能恢复的相关性具有一定参考意义。目的:探讨踝关节骨折术后踝穴冠状位角度变化对关节功能恢复的影响。方法:纳入进行手术治疗的86例踝关节骨折患者为研究对象,根据末次随访美国骨科足踝外科协会踝-后足评分结果分为优良组(n=45)和可差组(n=41),比较两组患者的一般资料。根据踝关节的踝穴位及侧位X射线片对比术后患者患侧和健侧的踝穴形态指标:包括踝穴宽度和深度、冠状位角度及矢状位角度,以及上述指标患侧和健侧之间的差值,并进一步进行组内比较分析。构建联合模型,利用Cox回归分析评估冠状位角度波动与关节功能恢复情况的关系。利用最小绝对收缩选择算子回归法和多因素Logistic回归分析影响患者关节功能恢复的危险因素。按踝穴冠状位角度从低到高等分为5分位数组(Q1-Q5),比较5组患者的临床资料特征,并采用多因素Logistic回归分析踝穴冠状位角度变化与关节功能恢复不良风险的相关性,建立限制性立方样条Logistic回归模型分析其剂量-反应关系。建立回归方程y=1-1/(1+e^(-z))预测模型并进行验证。结果与结论:①患者患侧的踝穴宽度和深度、冠状位角度及矢状位角度均显著大于健侧(P均<0.05);且与优良组患者相比,可差组患者踝穴宽度差值、深度差值、冠状位角度差值及矢状位角度差值均更大(P<0.05);②联合模型显示无论冠状位角度是否在正常范围内,冠状位角度每纵向增加1˚,关节功能恢复不良的风险增加3%;③最小绝对收缩选择算子回归和多因素Logistics回归分析显示,调整潜在混杂因素后发现年龄过大、早期功能锻炼缺乏、无跟骨牵引、内固定物未取出、术后并发症、踝冠状位角度增大均为影响患者关节功能恢复的独立危险因素(P<0.05);④术后3个月内的冠状位角度与关节功能恢复效果不良风险存在独立相关性(OR=1.57,95%CI:1.38-1.76,P=0.002),且术后各时间段冠状位角度从低到高5分位数组趋势性检验差异有统计学意义(P趋势<0.001);⑤限制性立方样条模型分析显示,男性或女性的踝穴冠状位角度变化与关节功能恢复效果不良风险均不存在非线性关系;经Bootstrap自抽样,预测模型区分度、准确度较好;⑥提示踝关节骨折术后踝穴冠状位角度减小对关节功能恢复起到明显的促进作用,因此在踝关节骨折术后重点检测踝穴冠状位角度有助于了解患者关节功能恢复情况。

关键词：踝关节骨折踝穴冠状位角度关节功能 Logistic回归分析

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3D imaging of the mitochondrial redox state of rathearts under normal and fasting conditions

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Journal of Innovative Optical Health Sciences 2014年第2期7卷 60-69页

作者： He N.Xu Rong zhou Lily Moon min Feng Lin z.Li Department of Radiology Universityof PennsyluaniaPhilade lphia PA 19104USA Briton Chance Laboratory of Redor Imaging Johnson Research Foundation Department of Biochemistry and Biophysics University of Pennsyluania Philade lphiaPA 19104USA Institute of Translational Medicine and Therapeutics Perelman School of Medicine University of Pennsylvania Philadelphia PA 19104USA

The heart requires continuous ATP availability that is generated in the *** using the cell culture and perfiused organ models have been carried out to investigate thebiochemistry in the mitochondria in response to a change in substrate supply,mitochondrialbioenergetics of heart under normal feed or fasting conditions has not been studied at the tissuelevel with a sub-millimeter spatial resolution either in vivo or er *** of many food-derived metabolites to generate ATP in the mitochondria is realized through the NADH/NAD+couple acting as a central electron *** employed the Chance redox scanner thelow-temperat ure fluorescence scanner to image the three-dimensional(3D)spatial distribution of themitochondrial redox states in heart tissues of rats under normai feeding or an overnight star-vation for 14.5 *** consecutive sections of each heart were imaged to map three redoxindices,i.e,NADH,oxidized favoproteins Fp,including flavin adenine dinucleotide(FAD)andthe redox ratio NADH/*** imaging results revealed the micro-heterogeneity and the spatial distribution of these redox *** quantitative analysis showed that in the fasted hearts thestandard deviation of both NADH and Fp,ie.,SD NADH and SDFp,significantly decreasedwith a p value of 0.032 and 0.045,respectively,indicating that the hearts become relatively morehomogeneous after *** fasted hearts contained 28.6%less NADH(p=0.038).No *** change in Fp was foumnd(p=0.4).The NADH/Fp ratio decreased with a marginalP value(0.076).The decreased NADH im the fasted hearts is consistent with the cardiac celsreliance of fatty acids consumption for energy metabolism when glucose becomes *** o bservation of N ADH decrease induced by dietary restriction in the heart at tissuelevel has not been reported to our best *** Chance redox scanner demonstrated thefeasibility of 3D imaging of the mitochondrial redox st ate in the heart and

关键词： Mitochondion metabolism bioenergetics cardiomyocyte NADH flavoproteins Fp FAD caloric restriction food deprivation.

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REDOX IMAGING OF THE p53-DEPENDENT MITOCHONDRIAL REDOX STATE IN COLON CANCER EX VIVO

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Journal of Innovative Optical Health Sciences 2013年第3期6卷 1-10页

作者： HE N.XU min FENG LILY MOON NATHAN DOLLOFF WAFIKEL-DEIRY LIN z.LI Department of Radiology University of Pennsylvania PhiladelphiaPAUSA Britton Chance Laboratory of Redox Imaging Johnson Research Foundation Department of Biochemistry and Biophysics Perelman School of Medicine University of Pennsylvania PhiladelphiaPAUSA Department of Medicine Penn State Hershey Medical Center and Penn State College of MedicineHersheyPAUSA Hematology/Oncology Penn State Hershey Medical Center HersheyPAUSA Abramson Cancer Center University of Pennsylvania PhiladelphiaPAUSA Institute of Translational Medicine and Therapeutics University of Pennsylvania PhiladelphiaPAUSA

The mitochondrial redox state and its heterogeneity of colon cancer at tissue level have not been previously *** has how p53 regulates mitochondial respi ration been measured at(deep)tissue level,presumably due to the unavailability of the technology that has sufficient spatial resolution and tissue penetration *** prior work demonstrated that the mito-chondrial redox state and its intnatumor heterogeneity is associated with cancer aggressiveness in human melanoma and breast cancer in mouse models,with the more metastatic tumons exhi-bit ing localized negions of more oxidized redox *** the Chance redox scanner with an in-plane spatial resolution of 200 pm,we imaged the mitochondrial redox state of the wild-type p53 colon tumors(HCT116 p53 ut)and the p5-deleted colon tumors(HCT116 p53-/-)by cllcting the fuorescence si gnals of nicotinamide adenine dimucleotide(NA DH)and oxidized flavoproteins [Fp,including favin adenine dinucleotide(FAD)]from the mouse xenogmafts snap frozen at low *** results show that:(1)both tumor lines have significant degree of intratumor heterogeneity of the redox state,typically exhibiting a distinct bi modal distribution that either correlates with the spatial core-rim pattern or the“hot/oold”oxida tion-roduction patches;.(2)the p531-group is significantly more beterogencous in the mitochondrial redox state and has a more oxidized turmor core compared to the p53 wt group when the tunor sizes of the two groups are matched;(3)the tumor size dependence of the redox indices(such as Fp and Fp redox ratio)is significant in the p531-group with the larger ones being more oxidized and more hetero-geneous in their redox state,particularly more oxidized in the tumor central regions;(4)the H&E staining images of tumor soctions grossly correlate with the redox *** present work is the first to reveal at the submillimeter scale the intratumor heterogeneity pattem of the mitochon-drial redox state in colon cancer and

关键词： NADH favoprotein intratumor heterogeneity HCT116 p53 null necrotic

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Flux variations of cosmic ray air showers detected by LHAASO-KM2A during a thunderstorm on June 10,2021

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Chinese Physics C 2023年第1期47卷 193-203页

作者： F.Aharonian 安琪阿西克古白立新白云翔包逸炜 D.Bastieri 毕效军毕玉江蔡金庭曹喆曹臻常进常劲帆陈恩生陈良陈亮陈龙陈明君陈玛丽陈素弘陈松战陈天禄陈学健陈阳程皓麟程宁程耀东崔树旺崔晓红崔昱东戴本忠代洪亮戴子高单增罗布 D.della Volpe 段凯凯樊军辉范一中范志香方军方堃冯存峰封莉冯少辉丰晓婷冯有亮高博高川东高林青高启高卫高伟康葛茂茂耿利斯龚光华苟全补顾旻皓郭福来郭俊广郭晓磊郭义庆郭莹莹韩毅昂何会海贺昊宁何思乐何新波何钰 M.Heller 贺远强侯超侯贤胡红波胡铨胡森胡世聪呼晓军黄代绘黄文昊黄性涛黄晓渊黄勇黄志成季筱璐贾焕玉贾康江琨姜泽军金敏康明铭柯通 D.Kuleshov 李兵兵李澄李骢李飞李海波李会财李华阳李军李剑李捷李凯李文龙李秀荣李昕李新李一卓李哲黎卓梁恩维梁云峰林苏杰刘冰刘成刘栋刘虎刘海东刘佳刘江来刘佳松刘金艳刘茂元柳若愚刘四明刘伟刘怡刘以农龙文杰鲁睿罗晴吕洪魁马伯强马玲玲马欣华毛基荣 A.Masood 闵振 W.Mitthumsiri 南云程区子维庞彬宇 P.Pattarakijwanich 裴致远齐孟尧祁业情乔冰强秦家军 D.Ruffolo A.Sáiz 邵澄宇邵琅 O.Shchegolev 盛祥东石京燕宋慧超 Yu.V.Stenkin V.Stepanov 苏扬孙秦宁孙晓娜孙志斌谭柏轩唐泽波田文武王博东王超王辉王洪光王建成王界双王利苹王玲玉王冉王润娜王为王祥高王祥玉王阳王玉东王岩谨王亚平王忠海王仲翔王振王铮韦大明魏俊杰魏永健文韬吴超勇吴含荣武莎吴雪峰吴雨生席邵强夏捷夏君集项光漫肖迪泫肖刚辛广广辛玉良邢祎熊峥徐东莲徐仁新薛良闫大海颜景志杨朝文杨冯帆杨何文杨佳盈杨莉莉杨明洁杨睿智杨深邦姚玉华姚志国叶一锰尹丽巧尹娜游晓浩游智勇于艳红袁强岳华曾厚敦曾婷轩曾玮曾宗康查敏翟徐徐张彬彬张丰张海明张恒英张建立张丽霞张力张路张鹏飞张佩佩张瑞张少博张少如张寿山张潇张笑鹏张云峰张月雷张毅张勇赵兵赵静赵雷赵立志赵世平郑福郑应周斌周浩周佳能周平周荣周勋秀祝成光祝凤荣朱辉朱科军左雄 Key Laboratory of Particle Astrophyics&Experimental Physics Division&Computing Center of Sciences Beijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institut for Nuclear Physics P.O.Box 10398069029 HeidelbergGermany State Key Laboratory of Particle Detection and Electronics China University of Science and Technology of China Hefei 230026China School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China College of Physics Sichuan UniversityChengdu 610065China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key Laboratory of Cosmic Rays(Tibet University) Ministry of Education850000 LhasaTibetChina National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China Hebei Normal University Shijiazhuang 050024China School of Physics and Astronomy(zhuhai)&School of Physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(zhuhai) Sun Yat-sen University519000 Zhuhai&510275 GuangzhouGuangdongChina Dipartimento di Fisica dell’Universitàdi Napoli"Federico II" Complesso Universitario di Monte Sant’Angelovia Cinthia80126 NapoliItaly School of Physics and Astronomy Yunnan UniversityKunming 650091China D´epartement de Physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde Genève24 Quai Ernest Ansermet1211 GenevaSwitzerland Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China Depar

The Large High Altitude Air Shower Observatory(LHAASO)has three sub-arrays,KM2A,WCDA,and *** flux variations of cosmic ray air showers were studied by analyzing the KM2A data during a thunderstorm on June 10,*** number of shower events that meet the trigger conditions increases significantly in atmospheric electric fields,with a maximum fractional increase of 20%.The variations in trigger rates(increases or decreases)were found to be strongly dependent on the primary zenith *** flux of secondary particles increased significantly,following a trend similar to that of shower *** better understand the observed behavior,Monte Carlo simulations were performed with CORSIKA and G4KM2A(a code based on GEANT4).We found that the experimental data(in saturated negative fields)were in good agreement with the simulations,assuming the presence of a uniform electric field of-700 V/cm with a thickness of 1500 m in the atmosphere above the observation *** to the acceleration/deceleration by the atmospheric electric field,the number of secondary particles with energy above the detector threshold was modified,resulting in the changes in shower detection rate.

关键词： thunderstorm cosmic rays extensive air showers LHAASO-KM2A

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The composite X-ray spectra of radio-loud and radio-quiet SDSS quasars

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Research in Astronomy and Astrophysics 2021年第1期21卷 33-44页

作者： min-Hua zhou min-Feng Gu Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy ofSciences80 Nandan RoadShanghai 200030China University of Chinese Academy of Sciences 19A Yuquan RoadBeijing 100049China

We present a study of the X-ray emission for a sample of radio-detected quasars constructed from the cross-matches between SDSS,FIRST catalogs and XMM-Newton archives.A sample of radio-quiet SDSS quasars without FIRST radio detection is also assembled for *** construct the optical and X-ray composite spectra normalized at rest frame 4215 A(or 2200 A)for both radio-loud quasars(RLQs)and radio-quiet quasars(RQQs)at z≤3.2,with matched X-ray completeness of 19%,redshift and optical *** the optical composite spectrum of RLQs is similar to that of RQQs,we find that RLQs have a higher X-ray composite spectrum than RQQs,consistent with previous studies in the *** dividing the radio-detected quasars into radio loudness bins,we find the X-ray composite spectra are generally higher with increasing radio ***,a significant correlation is found between the optical-to-X-ray spectral index and radio loudness,and there is a unified multi-correlation between the radio and X-ray luminosities and radio loudness in radio-detected *** results could be possibly explained with the corona-jet model,in which the corona and jet are directly related.

关键词： methods:statistical catalogs quasars:general X-rays:general

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