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Spectral and Timing Analysis of the Black Hole Transient MAxI J1631–479 during its 2019 Outburst Observed with Insight-HxMT

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Research in Astronomy and Astrophysics 2022年第11期22卷 21-33页

作者： yu-Cong Fu l.M.Song G.q.ding S.N.zhang J.l.qu S.zhang l.zhang q.C.Bu y.Huang x.Ma z.x.yang y.l.Tuo x.F.lu d.K.zhou B.y.Wu T.M.li y.C.xu xinjiang Astronomical Observatory Chinese Academy of SciencesUrumqiXinjiang 830011China University of Chinese Academy of Sciences Chinese Academy of SciencesBeijing 100049China Key laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China Institut fur Astronomie und Astrophysik Kepler Center for Astro and Particle PhysicsEberhard Karls UniversitatSand 1D-72076 TübingenGermany

We report spectral and timing analysis of the black hole transient MAxI J1631–479 during the hard intermediate state of its 2019 outburst from the Insight-Hard x-ray Modulation Telescope(Insight-HxMT)*** find that the energy dependence of the type-C quasi-periodic oscillation(qPO)frequency evolves with time:during the initial rise of a small flare(~MJd 58526.0-58527.1),the qPO frequency increases with increasing energy from~1 to~100 ke V,and then the frequency remains constant after MJd *** discover a possible new phenomenon of Fe line’s qPO frequency jump that has never been observed for other black hole transients:during the small flare,the qPO frequency around the Fe line energy is higher than any other energy band,with the frequency difference Δf=0.25±0.08 Hz between 5.5–7.5 ke V and other energy *** spectral analysis shows that the evolution of qPOs is related to the equivalent width of the narrow Fe line,and its equivalent width increases during this small *** propose that the qPO frequency difference results from the differential precession of a vertically extended jet,and the higher qPO frequency of Fe line could be caused by the layered jet when the jet scale *** the same time,the evolution of qPOs is related to the accretion rate,while the energy dependence of qPOs supports the existence of deceleration in the vertically distributed jet.

关键词： accretion accretion disks stars:black holes x-rays:binaries

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Optical readout uncooled infrared imaging detector using knife-edge filter operation

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Optoelectronics letters 2007年第2期3卷 119-122页

作者： zhang q MIAO z GUO z dong F xIONG z WU x CHEN d li C JIAO B Key laboratory of Mechanical Behavior and design of Materials University of Science and Technology of China Hefei 230027 China Institute of Microelectronics Chinese Academy of Science Beijing 100029 China

An optical readout uncooled infrared （IR） imaging detector of bimaterial cantilever array using knife-edge filter operation （KEFO） is demonstrated. The angle change of each cantilever in a focal plane array （FPA） can be simultaneously detected with a resolution of 10.5 degree. A deformation magnifying substrate-free micro-cantilever unit with multi-fold interval metaUized legs is specially designed and modeled. A FPA with 160×160 pixels is fabricated and thermal images with noise equivalent temperature difference （NETd） of 400 mK are obtained by this imaging detector.

关键词：光学读出非制冷红外成象探测器刀口滤波器运算设计模型

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Competition among the two-plasmon decay of backscattered light,filamentation of the electron-plasma wave and side stimulated Raman scattering

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High Power laser Science and Engineering 2023年第6期11卷 87-94页

作者： K.q.Pan z.C.li l.Guo T.Gong S.W.li d.y.ng C.y.zheng B.H.zhang x.T.He laser Fusion Research Center China Academy of Engineering PhysicsMianyangChina Center for Applied Physics and Technology Peking UniversityBeijingChina Institute of Applied Physics and Computational Mathematics BeijingChina

Competition among the two-plasmon decay(TPd)of backscattered light of stimulated Raman scattering(SRS),filamentation of the electron-plasma wave(EPW)and forward side SRS is investigated by two-dimensional particlein-cell *** previous work[*** et al.,*** 58,096035(2018)]showed that in a plasma with the density near 1/10 of the critical density,the backscattered light would excite the TPd,which results in suppression of the backward ***,this work further shows that when the laser intensity is so high(>10^(16)W/cm^(2))that the backward SRS cannot be totally suppressed,filamentation of the EPW and forward side SRS will be *** the TPd of the backscattered light only occurs in the early stage and is suppressed in the latter *** distribution functions further show that trapped-particle-modulation instability should be responsible for filamentation of the *** research can promote the understanding of hot-electron generation and SRS saturation in inertial confinement fusion experiments.

关键词： laser plasma instability inertial confinement fusion high energy density physics particle-in-cell simulation super-hot electrons

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Effects of chemical pressure on diluted magneticsemiconductor(Ba,K)(zn,Mn)_2As_2

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Chinese Physics B 2019年第5期28卷 288-292页

作者： y Peng S yu G q zhao W M li J F zhao l P Cao x C Wang q q liu S J zhang R z yu z deng x H zhu C q Jin College of Materials Science & Engineering Sichuan University Beijing National laboratory for Condensed Matter Physics and Institute of Physics Chinese Academy of Sciences School of Physics University of Chinese Academy of Sciences Collaborative Innovation Center of quantum Matter

Chemical pressure induced by iso-valent doping has been widely employed to tune physical properties of materials. In this work, we report effects of chemical pressure by substitution of Sb or P into As on a recently discovered diluted magnetic semiconductor(Ba,K)(zn,Mn)_2 As_2, which has the record of reliable Curie temperature of 230 K due to independent charge and spin doping. Sb and P are substituted into As-site to produce negative and positive chemical pressures, respectively.x-ray diffraction results demonstrate the successful chemical solution of dopants. Magnetic properties of both K-underdoped and K-optimal-doped samples are effectively tuned by Sb-and P-doping. The Hall effect measurements do not show decrease in carrier concentrations upon Sb-and P-doping. Impressively, magnetoresistance is significantly improved from7% to 27% by only 10% P-doping, successfully extending potential application of(Ba,K)(zn,Mn)_2 As_2.

关键词： chemical pressure (Ba,K)(zn,Mn)2As2 diluted magnetic semiconductor iso-valent doping

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STRUCTURAl dETERMINATION OF TITANIUM-OxIdE NANOPARTIClES By x-RAy ABSORPTION SPECTROSCOPy

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Acta Metallurgica Sinica(English letters) 2002年第1期15卷 53-57页

作者： z.y. Wu J. zhang K. Ibrahim M.I. Abbas G. li y. Tao T.d. Hu F.q. liu H.J. qian y.N. xie q.H. zhang l. Gao z.z. Chen Beijing Synchrotron Radiat. Facility Inst. of High Energy Phys. Chinese Acad. of Sci. Beijing 100039 China

As a potential application of titanium-oxide nanoparticles, it is extremely important to investigate a detailed picture of the surface and interior structural properties of nanocrystalline materials, such as rutile and anatase with diameters 7.0 and 4.5nm, respectively. x-ray absorption spectroscopy has been used to identify the local Ti environment and related electronic structure. We combine the experimental results at the Ti edge in both bulk and nano-crystals to determine the lattice distortion in terms of differently characteristic preedge features and the variation in the multiple-scattering region of x-ray absorption near-edge structure (xANES) spectra. The relationship between the transition peaks and the surface-to volume ratio is also discussed.

关键词： x-ray absorption near edge structure nano particle transition metal oxide

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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 Piazz.l. 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.l. z.l. z.l. 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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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

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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

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The design and performance of GRd onboard the GECAM satellite

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Radiation detection Technology and Methods 2022年第1期6卷 43-52页

作者： z.H.An x.l.Sun d.l.zhang S.yang x.q.li x.y.Wen K.Gong x.H.liang x.J.liu y.q.liu y.G.li S.l.xiong y.B.xu Fan zhang x.y.zhao C.Cai z.Chang G.Chen C.Chen y.y.du P.y.Feng M.Gao R.Gao d.y.Guo J.J.He d.J.Hou C.y.li G.li l.li x.F.li M.S.li 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 y.P.xu J.W.yang q.B.yi S.N.zhang C.y.zhang C.M.zhang Fei zhang y.zhao x.zhou CAS Institute of High Energy PhysicsBeijing 100049China State Key laboratory of Particle detection and Electronics Beijing 100049China 3 Xiangtan UniversityXiangtan 411105China 4 Beijing Normal UniversityBeijing 110875China xiangtan University Xiangtan 411105China Beijing Normal University Beijing 110875China

Background Each GECAM satellite payload contains 25 gamma-ray detectors(GRds),which can detect gamma-rays and particles and can roughly localize the Gamma-Ray Bursts(GRBs).GRd was designed using lanthanum bromide(laBr3)crystal as the sensitive material with the rear end coupled with silicon photomultiplier(SiPM)array for *** In aerospace engineering design of GRd,there are many key points to be *** this paper,we present the specific design scheme of GRd,the assembly and the performance test results of *** Based on Monte Carlo simulation and experimental test results,the specific schematic design and assembling process of GRd were *** being fully assembled,the GRds were conducted performance tests by using radioactive source and also conducted random vibration *** and conclusion The test results show that all satellite-borne GRds have energy resolutionquirements of satellite in scientific *** random vibration test shows that GRd can maintain in a stable performance,which meets the requirement of spatial application.

关键词： lanthanum bromide scintillator SiPM array GECAM Gamma-ray detector Energy resolution

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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 Piazz.l. 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.l. z.l. 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 d.y. 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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