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Probing the Bardeen-Kiselev black hole with the cosmological constant caused by Einstein equations coupled with nonlinear electrodynamics using quasinormal modes and greybody bounds

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Communications in Theoretical Physics 2024年第6期76卷 102-119页

作者： S R wu B Q wang Z w Long College of Physics Guizhou UniversityGuiyang 550025China College Pharmacy Guizhou University of Traditional Chinese MedicineGuiyang 550025China

In this work,we investigate a static and spherically symmetric Bardeen-Kiselev black hole(BH)with the cosmological constant,which is a solution of the Einstein-non-linear Maxwell field *** compute the quasinormal frequencies for the Bardeen-Kiselev BH with the cosmological constant due to electromagnetic and gravitational *** varying the BH parameters,we discuss the behavior of both real and imaginary parts of the BH quasinormal frequencies and compare these frequencies with the Reissner-Nordström-de Sitter BH surrounded by quintessence(RN-dSQ).Interestingly,it is shown that the responses of the Bardeen-Kiselev BH with the cosmological constant and the RN-dSQ under electromagnetic perturbations are different when the charge parameter q,the state parameter w and the normalization factor c are varied;however,for the gravitational perturbations,the responses of the Bardeen-Kiselev BH with the cosmological constant and the RN-dSQ are different only when the charge parameter q is ***,compared with the gravitational perturbations,the electromagnetic perturbations can be used to understand nonlinear and linear electromagnetic fields in curved spacetime *** interesting observation is that,due to the presence of Kiselev quintessence,the electromagnetic perturbations around the Bardeen-Kiselev BH with the cosmological constant damps faster and oscillates slowly;for the gravitational perturbations,the quasinormal mode decays slowly and oscillates *** also study the reflection and transmission coefficients along with the absorption cross section in the Bardeen-Kiselev BH with the cosmological constant;it is shown that the transmission coefficients will increase due to the presence of Kiselev quintessence.

关键词： quasinormal modes greybody factors Bardeen-Kiselev black hole with cosmological constant

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Geometrical reconstruction of fluorescence events observed by the LHAASO experiment

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Chinese Physics C 2021年第4期45卷 416-425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 H.Cai J.T.Cai Z.Cao Z.Cao J.Chang J.F.Chang x.C.Chang B.M.Chen J.Chen L.Chen L.Chen L.Chen M.J.Chen M.L.Chen Q.H.Chen S.H.Chen S.Z.Chen T.L.Chen x.L.Chen Y.Chen N.Cheng Y.D.Cheng S.w.Cui x.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu D.della Volpe B.DEtorre Piazzoli x.J.Dong J.H.Fan Y.Z.Fan Z.x.Fan J.Fang J.Fang C.F.Feng L.Feng S.H.Feng Y.L.Feng B.Gao C.D.Gao Q.Gao w.Gao M.M.Ge L.S.Geng G.H.Gong Q.B.Gou M.H.Gu J.G.Guo x.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He J.C.He S.L.He x.B.He Y.He M.Heller Y.K.Hor C.Hou x.Hou H.B.Hu S.Hu S.C.Hu x.J.Hu D.H.Huang Q.L.Huang w.H.Huang x.T.Huang Z.C.Huang F.Ji x.L.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.Levochkin B.B.Li C.Li C.Li F.Li H.B.Li H.C.Li H.Y.Li J.Li K.Li w.L.Li x.Li x.Li x.R.Li Y.Li Y.Z.Li Z.Li Z.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.L.Liu J.S.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu w.Liu Y.N.Liu Z.x.Liu w.J.Long R.Lu H.K.Lv B.Q.Ma L.L.Ma x.H.Ma J.R.Mao A.Masood w.Mitthumsiri T.Montaruli Y.C.Nan B.Y..Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Saiz L.Shao O.Shchegolev x.D.Sheng J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov 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.N.wang w.wang w.wang x.G.wang x.J.wang x.Y.wang Y.D.wang Y.J.wang Y.P.wang Z.wang Z.wang Z.H.wang Z.x.wang D.M.wei J.J.wei Y.J.wei T.wen C.Y.wu H.R.wu S.wu w.x.wu x.F.wu S.Q.xi J.xia J.J.xia G.M.xiang G.xiao H.B.xiao G.G.xin Y.L.xin Y.xing D.L.xu R.x.xu L.xue D.H.Yan C.w.Yang F.F.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.D.Zeng T.x.Zeng w.Zeng Z.K.Zeng M.Zha x.x.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.L.Zhang J.w.Zhang L.Zhang L.Zhang L.x.Zhang P.F.Zhang P.F.Zhang R.Zhang S.R.Zhang S.S.Zhang x.Zhang x.P.Zhang Y.Zhang Y.Zhang Y.F.Zhang Y.L.Zhang B.Zhao J.Zhao L.Zhao L.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou P 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 State Key Laboratory of Paricle Detection and Electronics China University of Science and Technology of China HefeiAnhui 230026China Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of Physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhouGuangdong 510006China School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhaiGuangdong 519000China School of Physical Science and Technology Guangxi UniversityNanningGuangxi 530004China Hebei Normal University ShijiazhuangHebei 050024China School of Physics and Microelectronics Zhengzhou UniversityZhengzhouHenan 450001China School of Astronomy and Space Science Nanjing UniversityNanjingJiangsu 210023China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjingJiangsu 210023China Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdaoShandong 266237China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and Technology Southwest Jiaotong UniversityChengduSichuan 610031China College of Physics Sichuan UniversityChengduSichuan 610065China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasaTibet 850000China School of physics and technology Wuhan UniversityWuhanHubei 430072Ch

The LHAASO-wFCTA experiment,which aims to observe cosmic rays in the sub-EeV range using the fluorescence technique,uses a new generation of high-performance *** ensure that the experiment has ex-cellent detection capability associated with the measurement of the energy spectrum,the primary composition of cosmic rays,and so on,an accurate geometrical reconstruction of air-shower events is *** paper de-scribes the development and testing of geometrical reconstruction for stereo viewed events using the wFCTA(wide Field of view Cherenkov/Fluorescence Telescope Array)*** approaches,which take full advantage ofthe wFCTA *** *** is the stereo-angular method,which uses the pointing of triggered SiPMs in the shower trajectory,and the other is the stereo-timing method,which uses the triggering time of the fired *** results show that both methods have good geometrical resolution:the resolution of the stereo-timing method is slightly better than the stereo-angular method because the resolution of the latter is slightly limited by the shower track length.

关键词： cosmic ray fluorescence telescope stereo observation geometrical reconstruction

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Observation of the Crab Nebula with LHAASO-KM2A−a performance study

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Chinese Physics C 2021年第2期45卷 518-530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 H.Cai J.T.Cai Z.Cao J.Chang J.F.Chang x.C.Chang B.M.Chen J.Chen L.Chen M.J.Chen M.L.Chen Q.H.Chen S.H.Chen S.Z.Chen T.L.Chen x.L.Chen Y.Chen N.Cheng Y.D.Cheng S.w.Cui x.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai D.della Volpe B.D'Ettorre Piazzoli x.J.Dong J.H.Fan Y.Z.Fan Z.x.Fan J.Fang K.Fang C.F.Feng L.Feng S.H.Feng Y.L.Feng B.Gao C.D.Gao Q.Gao w.Gao M.M.Ge L.S.Geng G.H.Gong Q.B.Gou M.H.Gu J.G.Guo x.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He J.C.He S.L.He x.B.He Y.He M.Heller Y.K.Hor C.Hou x.Hou H.B.Hu S.Hu S.C.Hu x.J.Hu D.H.Huang Q.L.Huang w.H.Huang x.T.Huang Z.C.Huang F.Ji x.L.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.Levochkin B.B.Li C.Li F.Li H.B.Li H.C.Li H.Y.Li J.Li K.Li w.L.Li x.Li x.R.Li Y.Li Y.Z.Li Z.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.N.Liu Z.x.Liu w.J.Long R.Lu H.K.Lv B.Q.Ma L.L.Ma x.H.Ma J.R.Mao A.Masood w.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Sáiz L.Shao O.Shchegolev x.D.Sheng J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov 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.N.wang w.wang x.G.wang x.J.wang x.Y.wang Y.D.wang Y.J.wang Y.P.wang Z.wang Z.H.wang Z.x.wang D.M.wei J.J.wei Y.J.wei T.wen C.Y.wu H.R.wu S.wu w.x.wu x.F.wu S.Q.xi J.xia J.J.xia G.M.xiang G.xiao H.B.xiao G.G.xin Y.L.xin Y.xing D.L.xu R.x.xu L.xue D.H.Yan C.w.Yang F.F.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.D.Zeng T.x.Zeng w.Zeng Z.K.Zeng M.Zha x.x.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.L.Zhang J.w.Zhang L.Zhang L.x.Zhang P.F.Zhang P.P.Zhang R.Zhang S.R.Zhang S.S.Zhang x.Zhang x.P.Zhang Y.Zhang Y.F.Zhang Y.L.Zhang B.Zhao J.Zhao L.Zhao L.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou P.Zhou R.Zhou x.x.Zhou C.G.Zhu F.R.Zhu H.Zhu K.J.Zhu x.Zuo Key Laboratory of Particle Astrophyics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of Sciences100049 BeijingChina University of Chinese Academy of Sciences 100049 BeijingChina TIANFU Cosmic Ray Research Center ChengduSichuanChina State Key Laboratory of Particle Detection and Electronics China University of Science and Technology of China 230026 HefeiAnhuiChina Department of Engineering Physics Tsinghua University100084 BeijingChina National Astronomical Observatories Chinese Academy of Sciences100101 BeijingChina National Space Science Center Chinese Academy of Sciences100190 BeijingChina School of Physics Peking University100871 BeijingChina Center for Astrophysics Guangzhou University510006 GuangzhouGuangdongChina School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen University519000 ZhuhaiGuangdongChina School of Physical Science and Technology Guangxi University530004 NanningGuangxiChina Hebei Normal University 050024 ShijiazhuangHebeiChina School of Physics and Microelectronics Zhengzhou University450001 ZhengzhouHenanChina School of Astronomy and Space Science Nanjing University210023 NanjingJiangsuChina Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of Sciences210023 NanjingJiangsuChina Institute of Frontier and Interdisciplinary Science Shandong University266237 QingdaoShandongChina Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of Sciences200030 ShanghaiChina Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong University200240 ShanghaiChina School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong University610031 ChengduSichuanChina College of Physics Sichuan University610065 ChengduSichuanChina Key Laboratory of Cosmic Rays(Tibet University) Ministry of Education850000 LhasaTibetChina School of Physics and Tec

A sub-array of the Large High Altitude Air Shower Observatory(LHAASO),KM2A is mainly designed to observe a large fraction of the northern sky to hunt for γ-ray sources at energies above 10 *** though the detector construction is still underway,half of the KM2A array has been operating stably since the end of *** this paper,we present the KM2A data analysis pipeline and the first observation of the Crab Nebula,a standard candle in very high energy γ-ray *** detect γ-ray signals from the Crab Nebula in both energy ranges of 10-100 TeV and>100 TeV with high significance,by analyzing the KM2A data of 136 live days between December 2019 and May *** the observations,we test the detector performance,including angular resolution,pointing accuracy and cosmic-ray background rejection *** energy spectrum of the Crab Nebula in the energy range 10-250 TeV fits well with a single power-law function dN/dE=(1.13±0.05stat±0.08sys)×10^(-14).(E/20 TeV)-309±0.06stat±0.02syscm^(-2) s^(-1) TeV^(-1).It is consistent with previous measurements by other *** opens a new window of γ-ray astronomy above 0.1 PeV through which new ultrahigh-energy γ-ray phenomena,such as cosmic PeVatrons,might be discovered.

关键词： γ-ray Crab Nebula extensive air showers cosmic rays

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Activation of LONP1 by 84-B10 alleviates aristolochic acid nephropathy via re-establishing mitochondrial and peroxisomal homeostasis

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Chinese Journal of Natural Medicines 2024年第9期22卷 808-821页

作者： xU x. ZHU w. MIAO M. BAI M. FAN J. NIU Y. LI Y. ZHANG A. JIA Z. wu M. School of Medicine Southeast University Nanjing 210009 China Department of Nephrology Children's Hospital of Nanjing Medical University Nanjing 210008 China Nanjing Key Laboratory of Pediatrics Children's Hospital of Nanjing Medical University Nanjing 210008 China Jiangsu Key Laboratory of Early Development and Chronic Diseases Prevention in Children Nanjing Medical University Nanjing 210029 China

Pharmaceutical formulations derived from Aristolochiaceae herbs, which contain aristolochic acids (AAs), are widely used for medicinal purposes. However, exposure to these plants and isolated AAs is linked to renal toxicity, known as AA nephropathy (AAN). Currently, the mechanisms underlying AAN are not fully understood, leading to unsatisfactory treatment strategies. In this study, we explored the protective role of 84-B10 (5-[[2-(4-methoxyphenoxy)-5-(trifluoromethyl) phenyl] amino]-5-oxo-3-phenylpentanoic acid) against AAN. RNA-seq analysis revealed that the mitochondrion and peroxisome were the most affected cellular components following 84-B10 treatment in AAN mice. Consistently, 84-B10 treatment preserved mitochondrial ultrastructure, restored mitochondrial respiration, enhanced the expression of key transporters (carnitine palmitoyltransferase 2) and enzymes (acyl-Coenzyme A dehydrogenase, medium chain) involved in mitochondrial fatty acid β-oxidation, and reduced mitochondrial ROS generation in both aristolochic acid I (AAI)-challenged mice kidneys and cultured proximal tubular epithelial cells. Additionally, 84-B10 treatment increased the expression of key transporters (ATP binding cassette subfamily D) and rate-limiting enzymes (acyl-CoA oxidase 1) involved in peroxisomal fatty acid β-oxidation and restored peroxisomal redox balance. Knocking down LONP1 expression diminished the protective effects of 84-B10 against AAN, suggesting LONP1-dependent protection. In conclusion, our study provides evidence that AAN is associated with significant disturbances in both mitochondrial and peroxisomal functions. The LONP1 activator 84-B10 demonstrates therapeutic potential against AAN, likely by maintaining homeostasis in both mitochondria and peroxisomes. © 2024 China Pharmaceutical University

关键词： 84-B10 Aristolochic acid nephropathy LONP1 Mitochondrion Peroxisome

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Line-of-shower trigger method to lower energy threshold for GRB detection using LHAASO-wCDA

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Radiation Detection Technology and Methods 2021年第4期5卷 531-541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 H.Cai J.T.Cai Z.Cao Z.Cao J.Chang J.F.Chang x.C.Chan B.M.Chen J.Chen L.Chen L.Chen L.Chen M.J.Chen M.L.Chen Q.H.Chen S.H.Chen S.Z.Chen T.L.Chen x.L.Chen Y.Chen N.Chen Y.D.Chen S.w.Cui x.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu D.della Volpe B.D’Ettorre Piazzoli x.J.Don J.H.Fan Y.Z.Fan Z.x.Fan J.Fang K.Fan C.F.Feng L.Feng S.H.Fen Y.L.Feng B.Gao C.D.Gao Q.Gao w.Gao M.M.Ge L.S.Gen G.H.Gong Q.B.Gou M.H.Gu J.G.Guo x.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He J.C.He S.L.He x.B.He Y.He M.Heller Y.K.Hor C.Hou x.Hou H.B.Hu S.Hu S.C.Hu x.J.Hu D.H.Huang Q.L.Huan w.H.Huang x.T.Huang Z.C.Huang F.Ji x.L.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.Levochkin B.B.Li C.Li C.Li F.Li H.B.Li H.C.Li H.Y.Li J.Li K.Li w.L.Li x.Li x.Li x.R.Li Y.Li Y.Z.Li Z.Li Z.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.N.Liu Z.x.Liu w.J.Long R.Lu H.K.Lv B.Q.Ma L.L.Ma x.H.Ma J.R.Mao A.Masood w.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Sáiz L.Shao O.Shchegolev x.D.Shen J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov Q.N.Sun x.N.Sun Z.B.Sun P.H.T.Tam Z.B.Tang w.w.Tian B.D.wan C.wang H.wang H.G.wang J.C.wang J.S.wang L.P.wang L.Y.wan R.N.wang w.wang w.wang x.G.wang x.J.wan x.Y.wang Y.D.wan Y.J.wan Y.P.wang Z.wang Z.wang Z.H.wang Z.x.wang D.M.wei J.J.wei Y.J.wei T.wen C.Y.wu H.R.wu S.wu w.x.wu x.F.wu S.Q.xi J.xia J.J.xia G.M.xiang G.xiao H.B.xiao G.G.xin Y.L.xin Y.xing D.L.xu R.x.xu L.xue D.H.Yan C.w.Yang F.F.Yang J.Y.Yang L.L.Yang M.J.Yan 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.D.Zeng T.x.Zeng w.Zeng Z.K.Zeng M.Zha x.x.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.L.Zhang J.w.Zhang L.Zhang L.Zhang L.x.Zhang P.F.Zhang P.P.Zhang R.Zhang S.R.Zhang S.S.Zhan x.Zhang x.P.Zhan Y.Zhan Y.Zhang Y.F.Zhang Y.L.Zhan B.Zhao J.Zhao L.Zhao L.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou P.Zhou R.Zhou x.x.Zhou C.G. 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 ChengduSichuanChina State Key Laboratory of Particle Detection and Electronics BeijingChina University of Science and Technology of China Hefei 230026AnhuiChina Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of Physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519000GuangdongChina School of Physical Science and Technology Guangxi UniversityNanning 530004GuangxiChina Hebei Normal University Shijiazhuang 050024HebeiChina School of Physics and Microelectronics Zhengzhou UniversityZhengzhou 450001HenanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of Physics Sichuan UniversityChengdu 610065SichuanChina Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina School of Physic

Purpose Observation of high energy and very high emission from Gamma Ray Bursts(GRBs)is crucial to study the gigantic explosion and the underline *** a large field-of-view and almost full duty cycle,the water Cherenkov Detector Array(wCDA),a sub-array of the Large High Altitude Air Shower Observatory(LHAASO),is appropriate to monitor the very high energy emission from unpredictable transients such as *** Nevertheless,the main issue for an extensive air shower array is the high energy threshold which limits the horizon of the *** address this issue a new trigger method is developed in this article to lower the energy threshold of wCDA for GRB *** The proposed method significantly improves the detection efficiency of wCDA for gamma-rays around the GRB direction at 10-300 *** sensitivity of the wCDA for GRB detection with the new trigger method is *** achieved sensitivity of the quarter wCDA array above 10 GeV is comparable with that of *** data analysis process and corresponding fluence upper limit for GRB 190719C is presented as an example.

关键词： LHAASO wCDA GRB

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weakly Supervised Object Localization with Background Suppression Erasing for Art Authentication and Copyright Protection

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Machine Intelligence Research 2024年第1期21卷 89-103页

作者： Chaojie wu Mingyang Li Ying Gao xinyan xie wing w.Y.Ng Ahmad Musyafa School of Computer Science and Engineering South China University of TechnologyGuangzhou 511442China Guangdong Provincial Key Laboratory of Artificial Intelligence in Medical Image Analysis and Application Guangdong Provincial People's HospitalGuangzhou 510180China

The problem of art forgery and infringement is becoming increasingly prominent,since diverse self-media contents with all kinds of art pieces are released on the Internet every *** art paintings,object detection and localization provide an efficient and ef-fective means of art authentication and copyright ***,the acquisition of a precise detector requires large amounts of ex-pensive pixel-level *** alleviate this,we propose a novel weakly supervised object localization(wSOL)with background su-perposition erasing(BSE),which recognizes objects with inexpensive image-level ***,integrated adversarial erasing(IAE)for vanilla convolutional neural network(CNN)dropouts the most discriminative region by leveraging high-level semantic ***,a background suppression module(BSM)limits the activation area of the IAE to the object region through a self-guidance ***,in the inference phase,we utilize the refined importance map(RIM)of middle features to obtain class-agnostic loc-alization *** experiments are conducted on paintings,CUB-200-2011 and ILSVRC to validate the effectiveness of our BSE.

关键词： weakly supervised object localization erasing method deep learning computer vision art authentication and copyright protection

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A dynamic range extension system for LHAASOwCDA-1

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Radiation Detection Technology and Methods 2021年第4期5卷 520-530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 H.Cai J.T.Cai Z.Cao Z.Cao J.Chang J.F.Chang x.C.Chang B.M.Chen J.Chen L.Chen L.Chen L.Chen M.J.Chen M.L.Chen Q.H.Chen S.H.Chen S.Z.Chen T.L.Chen x.L.Chen Y.Chen N.Cheng Y.D.Cheng S.w.Cui x.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu D.della Volpe B.D’Ettorre Piazzoli x.J.Dong J.H.Fan Y.Z.Fan Z.x.Fan J.Fang K.Fang C.F.Feng L.Feng S.H.Feng Y.L.Feng B.Gao C.D.Gao Q.Gao w.Gao M.M.Ge L.S.Geng G.H.Gong Q.B.Gou M.H.Gu J.G.Guo x.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He J.C.He S.L.He x.B.He Y.He M.Heller Y.K.Hor C.Hou x.Hou H.B.Hu S.Hu S.C.Hu x.J.Hu D.H.Huang Q.L.Huang w.H.Huang x.T.Huang Y.Huang Z.C.Huang F.Ji x.L.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.Levochkin B.B.Li C.Li C.Li F.Li H.B.Li H.C.Li H.Y.Li J.Li K.Li w.L.Li x.Li x.Li x.R.Li Y.Li Y.Z.Li Z.Li Z.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.N.Liu Z.x.Liu w.J.Long R.Lu H.K.Lv B.Q.Ma L.L.Ma x.H.Ma J.R.Mao A.Masood w.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Sáiz L.Shao O.Shchegolev x.D.Sheng J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov 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.N.wang w.wang w.wang x.G.wang x.J.wang x.Y.wang Y.D.wang Y.J.wang Y.P.wang Z.wang Z.wang Z.H.wang Z.x.wang D.M.wei J.J.wei Y.J.wei T.wen C.Y.wu H.R.wu S.wu w.x.wu x.F.wu S.Q.xi J.xia J.J.xia G.M.xiang G.xiao H.B.xiao G.G.xin Y.L.xin Y.xing D.L.xu R.x.xu L.xue D.H.Yan C.w.Yang F.F.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.D.Zeng T.x.Zeng w.Zeng Z.K.Zeng M.Zha x.x.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.L.Zhang J.w.Zhang L.Zhang L.Zhang L.x.Zhang P.F.Zhang P.P.Zhang R.Zhang S.R.Zhang S.S.Zhang x.Zhang x.P.Zhang Y.Zhang Y.Zhang Y.F.Zhang Y.L.Zhang B.Zhao J.Zhao L.Zhao L.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou 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 State Key Laboratory of Particle Detection and Electronics BeijingChina University of Science and Technology of China Hefei 230026AnhuiChina Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of Physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519000GuangdongChina School of Physical Science and Technology Guangxi UniversityNanning 530004GuangxiChina Hebei Normal University Shijiazhuang 050024HebeiChina School of Physics and Microelectronics Zhengzhou UniversityZhengzhou 450001HenanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of Physics Sichuan UniversityChengdu 610065SichuanChina Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina School of Physics

Purpose The main scientific goal of LHAASO-wCDA is to survey gamma-ray sources with energy from 100 GeV to 30 *** observe high-energy shower events,especially to measure the energy spectrum of cosmic rays from 100 TeV to 10 PeV,a dynamic range extension system(wCDA++)is designed to use a 1.5-inch PMT with a dynamic range of four orders of magnitude for each cell in *** The dynamic range is extended by using these PMTs to measure the effective charge density in the core region of air shower events,which is an important parameter for identifying the composition of primary *** and Conclusion The system has been running for more than one *** this paper,the details of the design and performance of wCDA++are presented.

关键词： LHAASO-wCDA wCDA++ water Cherenkov detector Performance

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Responses of growth performance,antioxidant function,small intestinal morphology and mRNA expression of jejunal tight junction protein to dietary iron in yellow-feathered broilers

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Journal of Integrative Agriculture 2024年第4期23卷 1329-1337页

作者： Kaiwen Lei Hao wu Jerry w Spears xi Lin xi wang xue Bai Yanling Huang Key Laboratory of Animal Science of State Ethnic Affairs Commission Southwest Minzu UniversityChengdu 610041China Key Laboratory of Qinghai-Tibetan Plateau Animal Genetic Resource Reservation and Utilization Southwest Minzu UniversityChengdu 610041China Department of Animal Science North Carolina State UniversityRaleighNC 27695-7621USA

This study aimed to investigate the dose-effect of iron on growth performance,antioxidant *** morphology,and mRNA expression of jejunal tight junction protein in 1-to21-d-old yellow-feathered broilers.A total of 7201-d-old yellow-feathered maleb roilers were allocated to 9 treatments with 8 replicate cages of 10 birds per *** dietary treatments were consisted of a basal diet(contained 79.6 mg Fe kg^(-1))supplemented with 0,20,40,60,80,160,320,640,and 1,280 mg Fe kg^(-1)in the form of FeSO_(4)·7H_(2)*** with the birds in the control group,birds supplemented with 20mg Fe kg^(-1)had higher average daily gain(ADG)(Pwith supplementation of 20mg Fe kg^(-1).Malondialdehyde(MDA)concentration in plasma and duodenum increased linearly(Pwith increased dietary Fe *** villus height(VH)in duodenum and jejunum,and the ratio of villus height to crypt depth(V/C)in duodenum decreased linearly(P?0.05)as dietary *** dietary Fe increased,the jejunal relative mRNA abundance of claudin-1 decreased linearly(P=0.001),but the jejunal relative mRNA abundance of zona occludens-1(ZO-1)and occludin decreased linearly(P?0.05)or quadratically(P?0.05).Compared with the supplementation of 20 mg Fe kg^(-1),the supplementation of640 mg Fe kg^(-1)or higher increased(P?0.05)MDA concentrations in plasma,duodenum,and jejunum,decreased VH in the duodenum and jejunum,and the addition of 1,280 mg Fe kg^(-1)reduced(P?0.05)the jejunal tight junction protein(claudin-1,ZO-1,occludin)mRNA *** summary,640 mg of supplemental Fe kg^(-1)or greater was associated with decreased growth performance,increased oxidative stress,disrupted intestinal morphology,and reduced mRNA expression of jejunal tight junction protein.

关键词： iron yellow-feathered broiler antioxidant function intestinal morphology tight junction protein

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Exploring impacts of COVID-19 on spatial and temporal patterns of visitors to Canadian Rocky Mountain National Parks from social media big data

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Journal of Forestry Research 2024年第4期35卷 13-33页

作者： Dehui Christina Geng Amy Li Jieyu Zhang Howie w.Harshaw Christopher Gaston wanli wu Guangyu wang National Park Research Centre Faculty of ForestryUniversity of British ColumbiaVancouver V6T 1Z4Canada Faculty of Applied Science University of British ColumbiaVancouver V6T 1Z3Canada Paul G.Allen School of Computer Science&Engineering University of WashingtonSeattleWA 98195USA Faculty of Kinesiology Sportand RecreationUniversity of AlbertaEdmonton T6G 2J9Canada Department of wood Science Faculty of ForestryUniversity of British ColumbiaVancouver V6T 1Z4Canada

COVID-19 posed challenges for global tourism *** in visitor temporal and spatial patterns and their associated determinants pre-and peri-pandemic in Canadian Rocky Mountain National Parks are *** was collected through social media programming and analyzed using spatiotemporal analysis and a geographically weighted regression(GwR)*** highlight that COVID-19 significantly changed park visitation *** tended to explore more remote areas *** GwR model also indicated distance to nearby trails was a significant influence on visitor *** results indicate that the pandemic influenced tourism temporal and spatial *** research presents a novel approach using combined social media big data which can be extended to the field of tourism management,and has important implications to manage visitor patterns and to allocate resources efficiently to satisfy multiple objectives of park management.

关键词： Tourism management Social media big data National parks COVID-19 Geographical weighted regression

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Performance of LHAASO-wCDA and observation of the Crab Nebula as a standard candle

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Chinese Physics C 2021年第8期45卷 166-181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 H.Cai J.T.Cai Z.Cao Z.Cao J.Chang J.F.Chang x.C.Chang B.M.Chen J.Chen L.Chen L.Chen L.Chen M.J.Chen M.L.Chen Q.H.Chen S.H.Chen S.Z.Chen T.L.Chen x.L.Chen Y.Chen N.Cheng Y.D.Cheng S.w.Cui x.H.Cui Y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu D.della Volpe B.D'Ettorre Piazzoli x.J.Dong J.H.Fan Y.Z.Fan Z.x.Fan J.Fang K.Fang C.F.Feng L.Feng S.H.Feng Y.L.Feng B.Gao C.D.Gao Q.Gao w.Gao M.M.Ge L.S.Geng G.H.Gong Q.B.Gou M.H.Gu J.G.Guo x.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He J.C.He S.L.He x.B.He Y.He M.Heller Y.K.Hor C.Hou x.Hou H.B.Hu S.Hu S.C.Hu x.J.Hu D.H.Huang Q.L.Huang w.H.Huang x.T.Huang Z.C.Huang F.Ji x.L.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.Levochkin B.B.Li C.Li C.Li F.Li H.B.Li H.C.Li H.Y.Li J.Li K.Li w.L.Li x.Li x.Li x.R.Li Y.Li Y.Z.Li Z.Li Z.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.N.Liu Z.x.Liu w.J.Long R.Lu H.K.Lv B.Q.Ma L.L.Ma x.H.Ma J.R.Mao A.Masood w.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi B.Q.Qiao D.Ruffolo V.Rulev A.Saiz L.Shao O.Shchegolev x.D.Sheng J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov 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.N.wang w.wang w.wang x.G.wang x.J.wang x.Y.wang Y.D.wang Y.J.wang Y.P.wang Z.wang Z.wang Z.H.wang Z.x.wang D.M.wei J.J.wei Y.J.wei T.wen C.Y.wu H.R.wu S.wu w.x.wu x.F.wu S.Q.xi J.xia J.J.xia G.M.xiang G.xiao H.B.xiao G.G.xin Y.L.xin Y.xing D.L.xu R.x.xu L.xue D.H.Yan C.w.Yang F.F.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.D.Zeng T.x.Zeng w.Zeng Z.K.Zeng M.Zha x.x.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.L.Zhang J.w.Zhang L.Zhang L.Zhang L.x.Zhang P.F.Zhang P.P.Zhang R.Zhang S.R.Zhang S.S.Zhang x.Zhang x.P.Zhang Y.Zhang Y.Zhang Y.F.Zhang Y.L.Zhang B.Zhao J.Zhao L.Zhao L.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou 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 State Key Laboratory of Particle Detection and Electronics China University of Science and Technology of China Hefei 230026China Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of Physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519082China School of Physical Science and Technology Guangxi UniversityNanning 530004China Hebei Normal University Shijiazhuang 050024China School of Physics and Microelectronics Zhengzhou UniversityZhengzhou 450001China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China College of Physics Sichuan UniversityChengdu 610065China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China School of Physics and Technology Wuhan UniversityWuhan 430072China School of Physics and Astronomy Yunnan University

The first water Cherenkov detector of the LHAASO experiment(wCDA-1)has been operating since April *** data for the first year have been analyzed to test its performance by observing the Crab Nebula as a standard *** wCDA-1 achieves a sensitivity of 65 mCU per year,with a statistical threshold of 5 *** accomplish this,a 97.7%cosmic-ray background rejection rate around 1 TeV and 99.8%around 6 TeV with an ap proximate photon acceptance of 50%is achieved after applying an algorithm to separate gamma-induced *** angular resolution is measured using the Crab Nebula as a point source to be approximately 0.45°at 1 TeV and better than 0.2°above 6 TeV,with a pointing accuracy better than 0.05°.These values all match the design *** energy resolution is found to be 33%for gamma rays around 6 *** spectral energy distribution of the Crab Nebula in the range from 500 GeV to 15.8 TeV is measured and found to be in agreement with the results from other TeV gamma ray observatories.

关键词： LHAASO-wCDA Crab Nebula angular resolution spectral energy distribution

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