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The Metastable Zone Width of Sodium Dichromate Dihydrate

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The Metastable Zone Width of Sodium Dichromate Dihydrate

CT上肿瘤-胸膜关系是周围型实性腺癌临床ⅠA期隐匿性淋巴结转移的危险因素

第十七届全国化学热力学和热分析学术会议

作者： l.p.wang Y.p.Dong J.Y.peng N.J.Dong H.T.Feng W.li Qinghai Institute of Salt lakes Chinese Academy of Sciences University of Chinese Academy of Sciences

Sodium dichromate dihydrate, one of the most important chromate compounds, can be widely used in wood preservation, leather tanning, metal finishing, and refractory.1-3 As a raw material, sodium dichromate dihydrate can also be used for the manufacture of both hexavalent and trivalent chromium products.4-5 The quality of these downstream products depends largely on the purity of sodium dichromate dihydrate. The high quality sodium dichromate dihydrate can be produced from industrial crystallization by operating crystallization conditions within the metastable zone throughout the crystallization process.6-8 Therefore, the investigation of Metastable Zone Width（MSZW） in terms of the separation and purification of sodium dichromate dihydrate is of theoretical and technological importance. In this work, polythermal method was used to determine the solubility and MSZW of sodium dichromate dihydrate, and thus the effects of cooling rate, initial composition on the MSZW have been investigated. In our experiment, five initial compositions of sodium dichromate dihydrate have been prepared and then crystallized at known cooling rates of 55, 45, 35, 25, and 15 K·h-1. The constant stirring rate was 450 rpm. The experimental MSZW data has been showed in Figure 1. It shows that the MSZW of sodium dichromate dihydrate narrows with the increase of initial composition. The reason is that the saturation temperature increases with the increase of initial composition, which improves the diffusion and collision probabilities of solute. As a result, the crystallization point goes ahead, thus the MSZW becomes narrow. However, there is an opposite effect of cooling rate on the MSZW of the sodium dichromate dihydrate. It may be seen from Figure 1 that the MSZW broadens with the increase of cooling rate. It is easy to explain that a higher cooling rate will supply a higher supercooling, which enhance the MSZW of sodium dichromate *** investigate the effect of stirring rates on the M

关键词： Metastable zone width Solubility Crystallization Sodium dichromate dihydrate

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国际医学放射学杂志 2023年第4期 487-488页

作者： C.Z.Zhang l.p.wang X.T.Cai M.F.li D.D.Sun p.wang 冉淑华

摘要目的探讨CT上的肿瘤-胸膜关系是否是周围型实性腺癌临床ⅠA期隐匿性淋巴结转移（OlNM）的危险因素。方法研究共纳入232例病人。肿瘤与胸膜的关系分为4

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增强乳腺X线摄影在乳腺导管原位癌术前检测中的作用：与低能量成像和MR成像的比较

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国际医学放射学杂志 2024年第4期 498-499页

作者： l.p.wang p.wang H.F.Shao J.li Q.l.Yang 高佳音

摘要目的比较对比增强乳腺X线摄影（CEM）与单独低能量成像（lEI）、CEM与MRI对乳腺导管原位癌（DCIS）的术前诊断价值。方法这项单中心回顾性研究分析了术前2

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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

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

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

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

Reconstruction of Cherenkov image bymultiple telescopes of lHAASO-WFCTA

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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

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