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The Lobster Eye Imager for Astronomy Onboard the SATech-01 Satellite

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Research in Astronomy and Astrophysics 2023年第9期23卷 66-78页

作者： z.x.Ling x.j.Sun c.zhang S.L.Sun G.jin S.N.zhang x.f.zhang j.B.chang f.S.chen Y.f.chen z.W.cheng W.fu Y.x.han h.Li j.f.Li Y.Li z.D.Li P.R.Liu Y.h.Lv x.h.ma Y.j.Tang c.B.Wang R.j.xie Y.L.xue A.L.Yan Q.zhang c.Y.Bao h.B.cai h.Q.cheng c.z.cui Y.f.Dai D.W.fan h.B.hu j.W.hu m.h.huang z.Q.jia c.c.jin D.Y.Li j.Q.Li h.Y.Liu m.j.Liu Y.Liu h.W.Pan Y.L.Qiu m.Sugizaki h.Sun W.x.Wang Y.L.Wang Q.Y.Wu x.P.xu Y.f.xu h.N.Yang x.Yang B.zhang m.zhang W.D.zhang z.zhang D.h.zhao x.Q.cong B.W.jiang L.h.Li x.B.Qiu j.N.Sun D.T.Su j.Wang c.Wu z.xu x.m.Yang S.K.zhang z.zhang N.zhang Y.f.zhu h.Y.Ban x.z.Bi z.m.cai W.chen x.chen Y.h.chen Y.cui x.L.Duan z.G feng Y.Gao j.W.he T.he j.j.huang f.Li j.S.Li T.j.Li T.T.Li h.Q.Liu L.Liu R.Liu S.Liu N.meng Q.Shi A.T.Sun Y.m.Wang Y.B.Wang h.c.Wu D.x xu Y.Q Yang Y.Yang x.S.Yu K.x.zhang Y.L.zhang Y.h.zhang Y.T.zhang h.zhou x.c.zhu j.S.cheng L.Qin L.Wang Q.L.Wang m.Bai R.L.Gao z.ji Y.R.Liu f.L.ma Y.j.Shi j.Su Y.Y.Tan j.z.Tong h.T.xu c.B.xue G.f.xue W.Yuan National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China Shanghai Institute of Technical Physics Chinese Academy of SciencesShanghai 200083China North Night Vision Technology co. LTDNanjing 211106China Institute of high Energy Physics Chinese Academy of SciencesBeijing 100049China Science and Technology on Low-Light-Level Night Vision Laboratory Xi'an 710065China Innovation Academy for microsatellites Chinese Academy of SciencesShanghai 201204China Institute of Electrical Engineering Chinese Academy of ScienceBeijing 100190China National Space Science center Chinese Academy of ScienceBeijing 100190China

The Lobster Eye Imager for Astronomy(LEIA),a pathfinder of the Wide-field x-ray Telescope of the Einstein Probe mission,was successfully launched onboard the SATech-01 satellite of the chinese Academy of Sciences on2022 july *** this paper,we introduce the design and on-ground test results of the LEIA *** stateof-the-art micro-Pore Optics(mPO),a wide field of view of 346 square degrees(18.6°×18.6°)of the x-ray imager is *** optical assembly composed of 36 mPO chips is used to focus incident x-ray photons,and four large-format complementary metal-oxide semiconductor(cmOS)sensors,each of size 6 cm×6 cm,are used as the focal plane *** instrument has an angular resolution of 4’-8’(in terms of fWhm)for the central focal spot of the point-spread function,and an effective area of 2-3 cm^(2) at 1 keV in essentially all the directions within the field of *** detection passband is 0.5-4 keV in soft x-rays and the sensitivity is2-3×10^(-11) erg s^(-1) cm^(-2)(about 1 millicrab)with a 1000 s *** total weight of LEIA is 56 kg and the power is 85 *** satellite,with a design lifetime of 2 yr,operates in a Sun-synchronous orbit of 500 km with an orbital period of 95 *** is paving the way for future missions by verifying in flight the technologies of both novel focusing imaging optics and cmOS sensors for x-ray observation,and by optimizing the working setups of the instrumental *** addition,LEIA is able to carry out scientific observations to find new transients and to monitor known sources in the soft x-ray band,albeit with limited useful observing time available.

关键词： instrumentation detectors-space vehicles instruments-telescopes-x-rays genera

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

STcf conceptual design report (Volume 1): Physics & detector

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frontiers of physics 2024年第1期19卷 1-154页

作者： m.Achasov x.c.Ai L.P.An R.Aliberti Q.An x.z.Bai Y.Bai O.Bakina A.Barnyakov V.Blinov V.Bobrovnikov D.Bodrov A.Bogomyagkov A.Bondar I.Boyko z.h.Bu f.m.cai h.cai j.j.cao Q.h.cao x.cao z.cao Q.chang K.T.chao D.Y.chen h.chen h.x.chen j.f.chen K.chen L.L.chen P.chen S.L.chen S.m.chen S.chen S.P.chen W.chen x.chen x.f.chen x.R.chen Y.chen Y.Q.chen h.Y.cheng j.cheng S.cheng T.G.cheng j.P.Dai L.Y.Dai x.c.Dai D.Dedovich A.Denig I.Denisenko j.m.Dias D.z.Ding L.Y.Dong W.h.Dong V.Druzhinin D.S.Du Y.j.Du z.G.Du L.m.Duan D.Epifanov Y.L.fan S.S.fang z.j.fang G.fedotovich c.Q.feng x.feng Y.T.feng j.L.fu j.Gao Y.N.Gao P.S.Ge c.Q.Geng L.S.Geng A.Gilman L.Gong T.Gong B.Gou W.Gradl j.L.Gu A.Guevara L.c.Gui A.Q.guo f.K.guo j.c.guo j.guo Y.P.guo z.h.guo A.Guskov K.L.han L.han m.han x.Q.hao j.B.he S.Q.he x.G.he Y.L.he z.B.he z.x.heng B.L.hou T.j.hou Y.R.hou c.Y.hu h.m.hu K.hu R.j.hu W.h.hu x.h.hu Y.c.hu j.hua G.S.huang j.S.huang m.huang Q.Y.huang W.Q.huang x.T.huang x.j.huang Y.B.huang Y.S.huang N.hüsken V.Ivanov Q.P.ji j.j.jia S.jia z.K.jia h.B.jiang j.jiang S.z.jiang j.B.jiao z.jiao h.j.jing x.L.Kang x.S.Kang B.c.Ke m.Kenzie A.Khoukaz I.Koop E.Kravchenko A.Kuzmin Y.Lei E.Levichev c.h.Li c.Li D.Y.Li f.Li G.Li G.Li h.B.Li h.Li h.N.Li h.j.Li h.L.Li j.m.Li j.Li L.Li L.Li L.Y.Li N.Li P.R.Li R.h.Li S.Li T.Li W.j.Li x.Li x.h.Li x.Q.Li x.h.Li Y.Li Y.Y.Li z.j.Li h.Liang j.h.Liang Y.T.Liang G.R.Liao L.z.Liao Y.Liao c.x.Lin D.x.Lin x.S.Lin B.j.Liu c.W.Liu D.Liu f.Liu G.m.Liu h.B.Liu j.Liu j.j.Liu j.B.Liu K.Liu K.Y.Liu K.Liu L.Liu Q.Liu S.B.Liu T.Liu x.Liu Y.W.Liu Y.Liu Y.L.Liu z.Q.Liu z.Y.Liu z.W.Liu I.Logashenko Y.Long c.G.Lu j.x.Lu N.Lu Q.f.Lü Y.Lu Y.Lu z.Lu P.Lukin f.j.Luo T.Luo x.f.Luo Y.h.Luo h.j.Lyu x.R.Lyu j.P.ma P.ma Y.ma Y.m.ma f.maas S.malde D.matvienko z.x.meng R.mitchell A.Nefediev Y.Nefedov S.L.Olsen Q.Ouyang P.Pakhlov G.Pakhlova x.Pan Y.Pan E.Passemar Y.P.Pei h.P.Peng L.Peng x.Y.Peng x.j.Peng K.Peters S.Pivovarov E.Pyata B.B.Qi Y.Q.Qi W.B.Qian Y.Qian c.f.Qiao j.j.Qin j.j.Qin L.Q.Qin x.S.Qin T.L.Qiu j.Rademacker c.f.Redmer h.Y.Sang Anhui University Hefei 230039China Beihang University Beijing 100191China Budker Institute of Nuclear Physics Novosibirsk 630090Russia cAS Key Laboratory of Theoretical Physics Institute of Theoretical PhysicsChinese Academy of SciencesBeijing 100190China cavendish Laboratory University of CambridgeJJ Thomson AveCambridge CB30HEUnited Kingdom central china Normal University Wuhan 430079China central South University Changsha 410083China china University of Geosciences Wuhan 430074China china University of mining and Technology Xuzhou 221116China École Polytechnique fédérale de Lausanne(EPfL) LausanneSwitzerland fudan University Shanghai 200433China Goethe University frankfurt D-60325 Frankfurt am MainGermany Guangxi Normal University Guilin 541004China Guangxi Uninversity Nanning 530004China hangzhou Institute for Advanced Study UCASHangzhou 310024China hebei Normal University Shijiazhuang 050024China hebei University Baoding 071002China hefei University of Technology Hefei 230601China helmholtz Institute mainz Staudinger Weg 18D-55099 MainzGermany henan Normal University Xinxiang 453007China henan University Kaifeng 475004China high Energy Physics center Chung-Ang UniversitySeoul 06974Korea higher School of Economy 11 Pokrovsky Bulvar Moscow 109028Russia huangshan University Huangshan 245000China hubei University of Automotive Technology Shiyan 442002China hunan Normal University Changsha 410081China hunan University of Science and Technology Xiangtan 411201China hunan University Changsha 410082China Indiana University BloomingtonIndiana 47405USA Inner mongolia University Hohhot 010021China Institute of Advanced Science facilities Shenzhen 518107China Institute of high Energy Physics Chinese Academy of SciencesBeijing 100049China Institute of modern Physics Chinese Academy of SciencesLanzhou 730000China Institute of Physics Academia SinicaTaipeiTaiwan 11529China Institute of Theoretical Physics Chinese Academy of SciencesBeijing 100190China jilin University Changch

The superτ-charm facility(STcf)is an electron–positron collider proposed by the chinese particle physics *** is designed to operate in a center-of-mass energy range from 2 to 7 GeV with a peak luminosity of 0.5×10^(35) cm^(–2)·s^(–1) or *** STcf will produce a data sample about a factor of 100 larger than that of the presentτ-charm factory—the BEPcII,providing a unique platform for exploring the asymmetry of matter-antimatter(charge-parity violation),in-depth studies of the internal structure of hadrons and the nature of non-perturbative strong interactions,as well as searching for exotic hadrons and physics beyond the Standard *** STcf project in china is under development with an extensive R&D *** document presents the physics opportunities at the STcf,describes conceptual designs of the STcf detector system,and discusses future plans for detector R&D and physics case studies.

关键词： electron–positron collider tau-charm region high luminosity STcf detector conceptual design

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

The design and performance of charged particle detector onboard the GEcAm mission

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Radiation Detection Technology and methods 2022年第1期6卷 53-62页

作者： Y.B.xu x.Q.Li x.L.Sun S.Yang h.Wang W.x.Peng x.h.Liang K.Gong Y.Q.Liu D.Y.guo x.Y.zhao c.Y.Li z.h.An j.j.he x.j.Liu x.Y.Wen S.L.xiong fan zhang D.L.zhang c.Y.zhang c.cai z.chang G.chen c.chen Y.Y.Du m.Gao R.Gao D.j.hou Y.G.Li G.Li L.Li x.f.Li m.S.Li f.j.Lu h.Lu B.meng f.Shi j.z.Wang Y.S.Wang h.z.Wang x.Wen S.xiao Y.P.xu j.W.Yang Q.B.Yi S.N.zhang c.m.zhang f.zhang Y.zhao x.zhou Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China

Background The Gravitational wave highly energetic Electromagnetic counterpart All-sky monitor(GEcAm)is dedicated to detecting gravitational wave gamma-ray *** is capable of all-sky monitoring over and discovering gamma-ray bursts and new radiation *** consists of two microsatellites,each equipped with 8 charged particle detectors(cPDs)and 25 gamma-ray detectors(GRDs).Purpose The cPD is used to measure charged particles in the space environment,monitor energy and flow intensity changes,and identify between gamma-ray bursts and space charged particle events in conjunction with *** cPD uses plastic scintillator as the sensitive material for detection,silicon photomultiplier array as the optically readable device,and the inlaid Am-241 radioactive source as the onboard calibration *** In this paper,we will present the working principle,physical design,functional implementation and preliminary performance test results of the *** a result,the energy range of electron,gamma-ray detection efficiency and dead time are tested to be better than the indexes required through the ground calibration experiment.

关键词： GEcAm cPD SiPm

Search for electron-antineutrinos associated with gravitational-wave events GW150914,GW151012,GW151226,GW170104,GW170608,GW170814,and GW170817 at Daya Bay

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chinese Physics c 2021年第5期45卷 190-201页

作者： f.P.An A.B.Balantekin h.R.Band m.Bishai S.Blyth G.f.cao j.cao j.f.chang Y.chang h.S.chen S.m.chen Y.chen Y.x.chen j.cheng z.K.cheng j.j.cherwinka m.c.chu j.P.cummings O.Dalager f.S.Deng Y.Y.Ding m.V.Diwan T.Dohnal j.Dove m.Dvorak D.A.Dwyer j.P.Gallo m.Gonchar G.h.Gong h.Gong W.Q.Gu j.Y.guo L.guo x.h.guo Y.h.guo z.guo R.W.hackenburg S.hans m.he K.m.heeger Y.K.heng A.higuera Y.K.hor Y.B.hsiung B.z.hu j.R.hu T.hu z.j.hu h.x.huang x.T.huang Y.B.huang P.huber D.E.jaffe K.L.jen x.L.ji x.P.ji R.A.johnson D.jones L.Kang S.h.Kettell S.Kohn m.Kramer T.j.Langford j.Lee j.h.c.Lee R.T.Lei R.Leitner j.K.c.Leung f.Li j.j.Li Q.j.Li S.Li S.c.Li W.D.Li x.N.Li x.Q.Li Y.f.Li z.B.Li h.Liang c.j.Lin G.L.Lin S.Lin j.j.Ling j.m.Link L.Littenberg B.R.Littlejohn j.c.Liu j.L.Liu c.Lu h.Q.Lu j.S.Lu K.B.Luk x.B.ma x.Y.ma Y.Q.ma c.marshall D.A.martinez caicedo K.T.meDonald R.D.mcKeown Y.meng j.Napolitano D.Naumov E.Naumova j.P.Ochoa-Ricoux A.OIshevskiy h.-R.Pan j.Park S.Patton j.c.Peng c.S.j.Pun f.z.Qi m.Qi x.Qian N.Raper j.Ren c.morales Reveco R.Rosero B.Roskovec x.c.Ruan h.Steiner j.L.Sun T.Tmej K.Treskov W.-h.Tse c.E.Tull B.Viren V.Vorobel c.h.Wang j.Wang m.Wang N.Y.Wang R.G.Wang W.Wang W.Wang x.Wang Y.Wang Y.f.Wang z.Wang z.Wang z.m.Wang h.Y.Wei L.h.Wei L.j.Wen K.Whisnant c.G.White h.L.h.Wong E.Worcester D.R.Wu f.L.Wu Q.Wu W.j.Wu D.m.xia z.Q.xie z.z.xing j.L.xu T.xu T.xue c.G.Yang L.Yang Y.z.Yang h.f.Yao m.Ye m.Yeh B.L.Young h.z.Yu z.Y.Yu B.B.Yue S.zeng Y.zeng L.zhan c.zhang f.Y.zhang h.h.zhang j.W.zhang Q.m.zhang x.T.zhang Y.m.zhang Y.x.zhang Y.Y.zhang z.j.zhang z.P.zhang z.Y.zhang j.zhao L.zhou h.L.zhuang j.h.zou Instiute of modern Physics East China University of Science and TechnologyShanghai 200237 University of Wisconsin MadisonWisconsin 53706 Wright Laboratory and Department of Physics Yale UniversityNew HavenConnecticut 06520 Brookhaven National Laboratory UptonNew York 11973 Department of Physics National Taiwan UniversityTaipei Institute of high Energy Physics Beijing 100049 National United University Miao-Li Department of Engineering Physics Tsinghua UniversityBejing 100084 Shenzhen University Shenzhen 518060 Sun Yat-Sen(zhongshan)University Guangzhou North china Electric Power University Bejjing 102206 chinese University of hong Kong Hong Kong 999077 Siena college LoudonvilleNew York 12211 Department of Physics and Astronomy University of CaliforniaIrvineCaliformia 92697 University of Science and Technology of china Hefei 230026 charles University Faculty of Mathematics and PhysicsPrague Department of Physics University of llinois at Urbana-ChampaignUrbanaIlinois 61801 Lawrence Berkeley National Laboratory BerkeleyCalifornia 94720 Department of Physics Illinois Institute of TechnologyChicagoIllinois 60616 joint Institute for Nuclear Research DubnaMoscow Region Beijing Normal University Beijing 100875 Department of Nuclear Science and Technology School of Energy and Power EngineeringXi'an Jiaotong UniversityXi'an 710049 Department of Physics University of HoustonHoustonTexas 77204 china Institute of Atomic Energy Beijing 102413 Shandong University Jinan 250100 Guangxi University Nanning 530004 center for Neutrino Physics Virginia TechBlacksburgVirginia 24061 Institute of Physics National Chiao-Tung UniversityHsinchu Department of Physics University of CincinnatiCincinnatiOhio 45221 Department of Physies Collge of Science and TechnologyTemple UniversityPhiladelphiaPennsylvania 19122 Dongguan University of Technology Dongguan 523808 Department of Physics University of CaliforniaBerkeleyCalifornia 94720 Department of Physics The University of Hong KongPokfulamHong Kong 999077 School

The establishment of a possible connection between neutrino emission and gravitational-wave(GW)bursts is important to our understanding of the physical processes that occur when black holes or neutron stars *** the Daya Bay experiment,using the data collected from December 2011 to August 2017,a search was per-formed for electron-antineutrino signals that coincided with detected GW events,including GW150914,GW151012,GW151226,GW170104,GW170608,GW 170814,and GW *** used three time windows of±10,±500,and±1000 s relative to the occurrence of the GW events and a neutrino energy range of 1.8 to 100 meV to search for correlated neutrino *** detected electron-antineutrino candidates were consistent with the expected background rates for all the three time *** monochromatic spectra,we found upper limits(90%confidence level)of the electron-antineutrino fluence of(1.13-2.44)×10^(11)cm^(-2)at 5 meV to 8.0×10^(7)cm^(-2)at 100 meV for the three time w *** the assumption of a fermi-Dirac spectrum,the upper limits were found to be(5.4-7.0)×10^(9)cm^(2)for the three time windows.

关键词： grav itational waves electron-antineutrinos fluence upper limit

Dedicated SiPm array for GRD of GEcAm

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Radiation Detection Technology and methods 2022年第1期6卷 63-69页

作者： D.L.zhang x.L.Sun z.h.An x.Q.Li x.Y.Wen K.Gong c.cai z.chang G.chen c.chen Y.Y.Du m.Gao R.Gao D.Y.guo j.j.he D.j.hou Y.G.Li c.Y.Li G.Li L.Li x.f.Li m.S.Li x.h.Liang x.j.Liu Y.Q.Liu f.j.Lu h.Lu B.meng W.x.Peng f.Shi h.Wang j.z.Wang Y.S.Wang h.z.Wang x.Wen S.xiao S.L.xiong Y.B.xu Y.P.xu S.Yang1 x.zhou j.W.Yang fan zhang S.N.zhang c.Y.zhang c.m.zhang fei zhang x.Y.zhao Institute of high Energy Physics CASBeijing 100049China State Key Laboratory of Particle Detection and Electronics Beijing 100049China

Purpose The discovery of gravitational waves and gamma-ray bursts heralds the era of multi-messenger *** the adoption of two small satellites to achieve the all-sky monitoring of gamma-ray bursts,the gravitational wave highenergy electromagnetic counterpart all-sky monitor(GEcAm)possesses a quasi-real-time early warning ability and plays an important role in positioning the sources of gravitational waves and in subsequent *** satellite of GEcAm was fitted with 253-inch-diameter gamma-ray detectors(GRD),covering an energy range of 8–2 *** have adopted silicon photomultiplier tubes(SiPm)in lieu of photomultiplier tubes(PmT)to adapt to the dimensional limitations of *** A unique 3-inch circular SiPm array was *** this design,646×6 mm chips were arranged evenly in a circular manner with the seams filled with reflecting films,thus achieving satisfactory uniformity of light *** integrated pre-amplifier circuit on the back of the SiPm array adopted two-level grouping and summing;further,it achieved a satisfactory signal-to-noise *** high-gain and low-gain channels were adopted to achieve a large dynamic range,and two independent power supply units were used,where each unit can be closed separately,thus improving *** Performance studies show that this SiPm array meets the requirements of *** A 3-inch SiPm array have been developed that uses grouped summation,reflective films,a circular arrangement,two groups of independent power supplies,high-and low-gain signals,differential signal output technologies,*** solution can be used not only for GEcAm,but also as a general solution for SiPm-based scintillation detectors.

关键词： SiPm GEcAm Gamma-ray Signal-to-noise ratio Reflecting film Pre-amplifier

The data acquisition algorithm designed for the SiPm-based detectors of GEcAm satellite

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Radiation Detection Technology and methods 2022年第1期6卷 70-77页

作者： Y.Q.Liu K.Gong x.Q.Li x.Y.Wen z.h.An c.cai z.chang G.chen c.chen Y.Y.Du m.Gao R.Gao D.Y.guo j.j.he D.j.hou Y.G.Li c.Y.Li G.Li L.Li x.f.Li m.S.Li x.h.Liang x.j.Liu f.j.Lu h.Lu B.meng W.x.Peng f.Shi x.L.Sun h.Wang j.z.Wang Y.S.Wang h.z.Wang x.Wen S.xiao S.L.xiong Y.B.xu Y.P.xu S.Yang j.W.Yang Q.B.Yi fan zhang D.L.zhang S.N.zhang c.Y.zhang c.m.zhang fei zhang x.Y.zhao Y.zhao x.zhou Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of chinese Academy of Sciences Chinese Academy of SciencesBeijing 100049China Physics and Space Science college China West Normal UniversityNanchong 637002China

Background The Gravitational Wave high-energy Electromagnetic counterpart All-sky monitor(GEcAm)consists of 2 microsatellites,each of which contains 25 GRD(LaBr3)detectors and 8 cPD(plastic scintillator)*** silicon photomultiplier(SiPm)array is used to read each *** output signal of these detectors with SiPm array is very special and challenging to *** this study,a novel data acquisition(DAQ)algorithm for these detectors is designed and implemented,and the content of the output event packet is *** and conclusion The performances,including the event acquisition efficiency of this DAQ algorithm,are extensively verified through experimental *** the on-ground and in-flight tests,this algorithm has excellent performance despite the very limited resources and short development time of GEcAm mission.

关键词： Silicon photomultiplier Digital waveform processing Data acquisition

Quality assurance test and failure analysis of SiPm arrays of GEcAm satellites

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Radiation Detection Technology and methods 2022年第1期6卷 35-42页

作者： D.L.zhang m.Gao x.L.Sun x.Q.Li z.h.An x.Y.Wen c.cai z.chang G.chen c.chen Y.Y.Du R.Gao K.Gong D.Y.guo j.j.he D.j.hou Y.G.Li c.Y.Li G.Li L.Li x.f.Li m.S.Li x.h.Liang x.j.Liu Y.Q.Liu f.j.Lu h.Lu B.meng W.x.Peng f.Shi h.Wang j.z.Wang Y.S.Wang h.z.Wang x.Wen S.xiao S.L.xiong Y.B.xu Y.P.xu S.Yang j.W.Yang fan.zhang S.N.zhang c.Y.zhang c.m.zhang fei zhang x.Y.zhao x.zhou Institute of high Energy Physics CASBeijing 100049People’s Republic of China

Background The Gravitational wave high-energy Electromagnetic counterpart All-sky monitor(GEcAm)satellite developed a SiPm-based gamma-ray detector to monitor the gravitational wave-related GRBs and guide subsequent observations in other wavelengths of *** As all the available SiPm devices belong to commercial grade,quality assurance tests need to be performed in accordance with the aerospace *** In the SiPm application of GEcAm,quality assurance experiments were *** mechanism of the failure of SiPm devices was analyzed during the development *** Based on the quality assurance test results,the fnal pass rate of SiPm array was 95%.Based on the failure analysis,it was found that a piece of SiPm had a leakage channel after longtime operation due to device *** According to the accumulated experience,in the reliability test of SiPm,it is necessary to pay special attention to test the impedance of each pin of SiPm to ground and confrm that the power switch state of SiPm is controllable.

关键词： Gravitational waves Gamma-ray detectors Silicon photomultipliers Quality assurance test failure analysis