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First-and second-order phase transitions in RE_(6)Co_(2)Ga(RE=Ho,Dy or Gd)cryogenic magnetocaloric materials

science China Materials 2021年第11期64卷 2846-2857页

作者： Dan Guo luis M.Moreno-Ramírez Carlos Romero-Muñiz Yikun Zhang Jia-Yan law Victorino Franco Jiang Wang Zhongming Ren state Key laboratory of Advanced special steels Shanghai Key Laboratory of Advanced FerrometallurgySchool of Materials Science and EngineeringShanghai UniversityShanghai 200072China Departamento de Física de la Materia Condensada ICMS-CSICUniversidad de SevillaP.O.Box 1065Sevilla 41080Spain Department of Physical Chemical and Natural SystemsUniversidad Pablo de OlavideSevilla E-41013Spain Departamento de Física Aplicada I Universidad de SevillaSevilla E-41012Spain

Rare-earth(RE)rich intermetallics crystallizing in orthorhombic Ho_(6)Co_(2)Ga-type crystal structure exhibit peculiar magnetic properties that are not widely reported for their magnetic ordering,order of magnetic phase transition,and related magnetocaloric *** tuning the type of RE element in RE_(6)Co_(2)Ga(RE=Ho,Dy or Gd)compounds,metamagnetic anti-to-paramagnetic(AF to PM)phase transitions could be tuned to ferro-to-paramagnetic(FM to PM)phase ***,the FM ground state for Gd_(6)Co_(2)Ga is confirmed by density functional theory calculations in addition to experimental *** field dependence magnetocaloric and Banerjee’s criteria demonstrate that Ho_(6)Co_(2)Ga and Dy_(6)Co_(2)Ga undergo a first-order phase transition in addition to a second-order phase transition,whereas only the latter is observed for Gd_(6)Co_(2)*** two extreme alloys of the series,Ho_(6)Co_(2)Ga and Gd_(6)Co_(2)Ga,show maximum isothermal entropy change(|Δs_(iso)^(max)(5T)|)of 10.1 and 9.1 J kg^(-1)K^(-1)at 26 and 75 K,close to H_(2)and N_(2)liquefaction,*** outstanding magnetocaloric effect performance makes the RE6 Co_(2)Ga series of potential for cryogenic magnetic refrigeration applications.

关键词： RE6Co2Ga compounds magnetic phase transitions magnetocaloric effect rare-earth

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

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Chinese Physics C 2021年第2期45卷 518-530页

作者： F.Aharonian Q.An Axikegu l.X.Bai Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi H.Cai J.T.Cai Z.Cao J.Chang J.F.Chang X.C.Chang B.M.Chen J.Chen l.Chen M.J.Chen M.l.Chen Q.H.Chen s.H.Chen s.Z.Chen T.l.Chen X.l.Chen Y.Chen N.Cheng Y.D.Cheng s.W.Cui X.H.Cui Y.D.Cui B.Z.Dai H.l.Dai Z.G.Dai D.della Volpe B.D'Ettorre Piazzoli X.J.Dong J.H.Fan Y.Z.Fan Z.X.Fan J.Fang K.Fang C.F.Feng l.Feng s.H.Feng Y.l.Feng B.Gao C.D.Gao Q.Gao W.Gao M.M.Ge l.s.Geng G.H.Gong Q.B.Gou M.H.Gu J.G.Guo X.l.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He J.C.He s.l.He X.B.He Y.He M.Heller Y.K.Hor C.Hou X.Hou H.B.Hu s.Hu s.C.Hu X.J.Hu D.H.Huang Q.l.Huang W.H.Huang X.T.Huang Z.C.Huang F.Ji X.l.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.levochkin B.B.li C.li F.li H.B.li H.C.li H.Y.li J.li K.li W.l.li X.li X.R.li Y.li Y.Z.li Z.li E.W.liang Y.F.liang s.J.lin B.liu C.liu D.liu H.liu H.D.liu J.liu J.l.liu J.s.liu J.Y.liu M.Y.liu R.Y.liu s.M.liu W.liu Y.N.liu Z.X.liu W.J.long R.lu H.K.lv B.Q.Ma l.l.Ma X.H.Ma J.R.Mao A.Masood W.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev a.s.iz.l.s.ao O.shchegolev X.D.sheng J.R.shi H.C.song Yu.V.stenkin V.stepanov Q.N.sun X.N.sun Z.B.sun P.H.T.Tam Z.B.Tang W.W.Tian B.D.Wang C.Wang H.Wang H.G.Wang J.C.Wang J.s.Wang l.P.Wang l.Y.Wang R.N.Wang W.Wang X.G.Wang X.J.Wang X.Y.Wang Y.D.Wang Y.J.Wang Y.P.Wang Z.Wang Z.H.Wang Z.X.Wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.Wu H.R.Wu s.Wu W.X.Wu X.F.Wu s.Q.Xi J.Xia J.J.Xia G.M.Xiang G.Xiao H.B.Xiao G.G.Xin Y.l.Xin Y.Xing D.l.Xu R.X.Xu l.Xue D.H.Yan C.W.Yang F.F.Yang J.Y.Yang l.l.Yang M.J.Yang R.Z.Yang s.B.Yang Y.H.Yao Z.G.Yao Y.M.Ye l.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.D.Zeng T.X.Zeng W.Zeng Z.K.Zeng M.Zha X.X.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.l.Zhang J.W.Zhang l.Zhang l.X.Zhang P.F.Zhang P.P.Zhang R.Zhang s.R.Zhang s.s.Zhang X.Zhang X.P.Zhang Y.Zhang Y.F.Zhang Y.l.Zhang B.Zhao J.Zhao l.Zhao l.Z.Zhao s.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou P.Zhou R.Zhou X.X.Zhou C.G.Zhu F.R.Zhu H.Zhu K.J.Zhu X.Zuo Key laboratory of Particle Astrophyics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of Sciences100049 BeijingChina University of Chinese Academy of sciences 100049 BeijingChina TIANFU Cosmic Ray Research Center ChengduSichuanChina state Key laboratory of Particle Detection and Electronics China University of science and Technology of China 230026 HefeiAnhuiChina Department of Engineering Physics Tsinghua University100084 BeijingChina National Astronomical Observatories Chinese Academy of Sciences100101 BeijingChina National space science Center Chinese Academy of Sciences100190 BeijingChina school of Physics Peking University100871 BeijingChina Center for Astrophysics Guangzhou University510006 GuangzhouGuangdongChina school of Physics and Astronomy&school of Physics(Guangzhou) Sun Yat-sen University519000 ZhuhaiGuangdongChina school of Physical science and Technology Guangxi University530004 NanningGuangxiChina Hebei Normal University 050024 ShijiazhuangHebeiChina school of Physics and Microelectronics Zhengzhou University450001 ZhengzhouHenanChina school of Astronomy and space science Nanjing University210023 NanjingJiangsuChina Key laboratory of Dark Matter and space Astronomy Purple Mountain ObservatoryChinese Academy of Sciences210023 NanjingJiangsuChina Institute of Frontier and Interdisciplinary science Shandong University266237 QingdaoShandongChina Key laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of Sciences200030 ShanghaiChina Tsung-Dao lee Institute&school of Physics and Astronomy Shanghai Jiao Tong University200240 ShanghaiChina school of Physical science and Technology&school of Information science and Technology Southwest Jiaotong University610031 ChengduSichuanChina College of Physics Sichuan University610065 ChengduSichuanChina Key laboratory of Cosmic Rays(Tibet University) Ministry of Education850000 LhasaTibetChina school of Physics and Tec

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

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

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Relaxor ferroelectric behavior:An approach considering both the dipolar and electrical conductivity contributions

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Journal of Advanced Dielectrics 2021年第3期11卷 51-55页

作者： C.Carreras-Casas O.García-Zaldívar A.Peláiz-Barranco Y.González-Abreu F.Calderón-Pinar J.D.s.Guerra Grupo de Materiales Ferroicos Facultad de Física-Instituto de Ciencia y Tecnología de Materiales Universidad de la Habana La Habana 10400Cuba Grupo de Ferroelétricos e Materiais Multifuncionais Instituto de Física Universidade Federal de Uberlandia UberlandiaMinas Gerais38408-100Brazil

The relaxor behavior of PlZT ferroelectric ceramics has been analyzed in a wide frequency and temperature ranges,below and above the temperature for the formation of the so-called polar nano-regions(PNRs).An approximation to the dynamical behavior of the PNRs has been discussed using Cole-Cole’s relaxation model and Jonscher’s Universal Relaxation *** analysis considers both the dipolar contribution and those ones associated with DC and AC electric conductivities,this latter not being previously reported in the literature for relaxor *** effectiveness of the developed model has been verified from the agreement between the experimental data and the theoretical *** study also offers an indirect method to predict the DC component of the electrical conductivity.

关键词： Relaxor ferroelectrics dielectric response modeling conductivity Cole-Cole

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Arsenite provides a selective signal that coordinates arsenate uptake and detoxification through the regulation of PHR1 stability in Arabidopsis

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Molecular Plant 2022年第11期15卷 1826-1826页

作者： Cristina Navarro Cristian Mateo-Elizalde Thotegowdanapalya CMohan Eduardo sánchez-Bermejo Oscar Urrutia María Nieves Fernández-Muñiz JoséMGarcía-Mina Riansares Muñoz Javier Paz-Ares Gabriel Castrillo Antonio leyva 不详

(Molecular Plant 14,1489-1507;september 6,2021)In the“Accession numbers”section in the originally published version of our manuscript,we mistakenly listed At5g44570 as the Arabidopsis Genome Initiative locus identif... 详细信息

关键词： Arabidopsis identifier stability

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The long Way from Complex Phenotypes to Genes: The story of Rat Chromosome 4 and Its Behavioral Effects

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World Journal of Neuroscience 2014年第3期4卷 203-215页

作者： Gabriela Ferreira de Medeiros Fernanda Junkes Corrêa María Elisa Corvino Geison de souza izídio André Ramos laboratório de Genética do Comportamento Departamento de Biologia Celular Embriologia e Genética Universidade Federal de Santa Catarina Florianópolis Brazil

Quantitative trait loci (QTls) mapping has been performed during the past decades in an attempt to identify genes, gene products and mechanisms underlying numerous quantitative traits. It’s a strategy based on natural variations in genes and gene products, which facilitates translation from animal models to human clinical conditions. Our team has shown that the inbred rat strains lewis (lEW) and spontaneously Hypertensive Rats (sHR) differ with respect to several emotionality- related behaviors, one of which (inner locomotion in the open field) was strongly influenced by a QTl (Anxrr16) on rat chromosome 4. since then, several other studies not only corroborated the initial description of Anxrr16, but also extrapolated its effects to a broader context (rats from both sexes and regardless of the estrous cycle phase) and suggested that this same region influences other emotionality-related behaviors as well as alcohol intake. Other QTls affecting neurobiological traits were also found on rat chromosome 4 and several candidate genes have been pointed out as possibly influencing those phenotypes. Altogether, these studies suggest that rat chromosome 4 constitutes an interesting target for the study of the molecular bases of anxiety and other traits related to emotional reactivity.

关键词： Rat Chromosome 4 QTl Anxrr16 Emotionality-Related Behaviors Alcohol Consumption stress-Response

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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

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line-of-shower trigger method to lower energy threshold for GRB detection using lHAAsO-WCDA

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Radiation Detection Technology and Methods 2021年第4期5卷 531-541页

作者： F.Aharonian Q.An Axikegu l.X.Bai Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi H.Cai J.T.Cai Z.Cao Z.Cao J.Chang J.F.Chang X.C.Chan B.M.Chen J.Chen l.Chen l.Chen l.Chen M.J.Chen M.l.Chen Q.H.Chen s.H.Chen s.Z.Chen T.l.Chen X.l.Chen Y.Chen N.Chen Y.D.Chen s.W.Cui X.H.Cui Y.D.Cui B.Z.Dai H.l.Dai Z.G.Dai Danzengluobu D.della Volpe B.D’Ettorre Piazzoli X.J.Don J.H.Fan Y.Z.Fan Z.X.Fan J.Fang K.Fan C.F.Feng l.Feng s.H.Fen Y.l.Feng B.Gao C.D.Gao Q.Gao W.Gao M.M.Ge l.s.Gen G.H.Gong Q.B.Gou M.H.Gu J.G.Guo X.l.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He J.C.He s.l.He X.B.He Y.He M.Heller Y.K.Hor C.Hou X.Hou H.B.Hu s.Hu s.C.Hu X.J.Hu D.H.Huang Q.l.Huan W.H.Huang X.T.Huang Z.C.Huang F.Ji X.l.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.levochkin B.B.li C.li C.li F.li H.B.li H.C.li H.Y.li J.li K.li W.l.li X.li X.li X.R.li Y.li Y.Z.li Z.li Z.li E.W.liang Y.F.liang s.J.lin B.liu C.liu D.liu H.liu H.D.liu J.liu J.l.liu J.s.liu J.Y.liu M.Y.liu R.Y.liu s.M.liu W.liu Y.N.liu Z.X.liu W.J.long R.lu H.K.lv B.Q.Ma l.l.Ma X.H.Ma J.R.Mao A.Masood W.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev a.s.iz.l.s.ao O.shchegolev X.D.shen J.R.shi H.C.song Yu.V.stenkin V.stepanov Q.N.sun X.N.sun Z.B.sun P.H.T.Tam Z.B.Tang W.W.Tian B.D.Wan C.Wang H.Wang H.G.Wang J.C.Wang J.s.Wang l.P.Wang l.Y.Wan R.N.Wang W.Wang W.Wang X.G.Wang X.J.Wan X.Y.Wang Y.D.Wan Y.J.Wan Y.P.Wang Z.Wang Z.Wang Z.H.Wang Z.X.Wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.Wu H.R.Wu s.Wu W.X.Wu X.F.Wu s.Q.Xi J.Xia J.J.Xia G.M.Xiang G.Xiao H.B.Xiao G.G.Xin Y.l.Xin Y.Xing D.l.Xu R.X.Xu l.Xue D.H.Yan C.W.Yang F.F.Yang J.Y.Yang l.l.Yang M.J.Yan R.Z.Yang s.B.Yang Y.H.Yao Z.G.Yao Y.M.Ye l.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.D.Zeng T.X.Zeng W.Zeng Z.K.Zeng M.Zha X.X.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.l.Zhang J.W.Zhang l.Zhang l.Zhang l.X.Zhang P.F.Zhang P.P.Zhang R.Zhang s.R.Zhang s.s.Zhan X.Zhang X.P.Zhan Y.Zhan Y.Zhang Y.F.Zhang Y.l.Zhan B.Zhao J.Zhao l.Zhao l.Z.Zhao s.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou P.Zhou R.Zhou X.X.Zhou C.G. Key laboratory of Particle Astrophysics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina state Key laboratory of Particle Detection and Electronics BeijingChina University of science and Technology of China Hefei 230026AnhuiChina Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National space science Center Chinese Academy of SciencesBeijing 100190China school of Physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina school of Physics and Astronomy&school of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519000GuangdongChina school of Physical science and Technology Guangxi UniversityNanning 530004GuangxiChina Hebei Normal University Shijiazhuang 050024HebeiChina school of Physics and Microelectronics Zhengzhou UniversityZhengzhou 450001HenanChina school of Astronomy and space science Nanjing UniversityNanjing 210023JiangsuChina Key laboratory of Dark Matter and space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of Frontier and Interdisciplinary science Shandong UniversityQingdao 266237ShandongChina Key laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao lee Institute&school of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China school of Physical science and Technology&school of Information science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of Physics Sichuan UniversityChengdu 610065SichuanChina Key laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina school of Physic

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

关键词： lHAAsO WCDA GRB

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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.s.iz.l.s.ao O.shchegolev X.D.sheng J.R.shi H.C.song Yu.V.stenkin V.stepanov Q.N.sun X.N.sun Z.B.sun P.H.T.Tam Z.B.Tang W.W.Tian B.D.Wang C.Wang H.Wang H.G.Wang J.C.Wang J.s.Wang l.P.Wang l.Y.Wang R.N.Wang W.Wang W.Wang X.G.Wang X.J.Wang X.Y.Wang Y.D.Wang Y.J.Wang Y.P.Wang Z.Wang Z.Wang Z.H.Wang Z.X.Wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.Wu H.R.Wu s.Wu W.X.Wu X.F.Wu s.Q.Xi J.Xia J.J.Xia G.M.Xiang G.Xiao H.B.Xiao G.G.Xin Y.l.Xin Y.Xing D.l.Xu R.X.Xu l.Xue D.H.Yan C.W.Yang F.F.Yang J.Y.Yang l.l.Yang M.J.Yang R.Z.Yang s.B.Yang Y.H.Yao Z.G.Yao Y.M.Ye l.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.D.Zeng T.X.Zeng W.Zeng Z.K.Zeng M.Zha X.X.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.l.Zhang J.W.Zhang l.Zhang l.Zhang l.X.Zhang P.F.Zhang P.P.Zhang R.Zhang s.R.Zhang s.s.Zhang X.Zhang X.P.Zhang Y.Zhang Y.Zhang Y.F.Zhang Y.l.Zhang B.Zhao J.Zhao l.Zhao l.Z.Zhao s.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou Key laboratory of Particle Astrophyics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina state Key laboratory of Particle Detection and Electronics BeijingChina University of science and Technology of China Hefei 230026AnhuiChina Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National space science Center Chinese Academy of SciencesBeijing 100190China school of Physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina school of Physics and Astronomy&school of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519000GuangdongChina school of Physical science and Technology Guangxi UniversityNanning 530004GuangxiChina Hebei Normal University Shijiazhuang 050024HebeiChina school of Physics and Microelectronics Zhengzhou UniversityZhengzhou 450001HenanChina school of Astronomy and space science Nanjing UniversityNanjing 210023JiangsuChina Key laboratory of Dark Matter and space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of Frontier and Interdisciplinary science Shandong UniversityQingdao 266237ShandongChina Key laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao lee Institute&school of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China school of Physical science and Technology&school of Information science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of Physics Sichuan UniversityChengdu 610065SichuanChina Key laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina school of Physics

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

关键词： lHAAsO-WCDA WCDA++ Water Cherenkov detector Performance

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Prospects for a multi-TeV gamma-ray sky survey with the lHAAsO water Cherenkov detector array

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Chinese Physics C 2020年第6期44卷 123-132页

作者： F.Aharonian V.Alekseenko Q.An Axikegu l.X.Bai Y.W.Bao D.Bastieri9 X.J.Bi H.Cai Zhe Cao Zhen Cao J.Chang J.F.Chang X.C.Chang s.P.Chao B.M.Chen J.Chen l.Chen l.Chen M.l.Chen M.J.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 B.D'Ettorre Piazzoli J.Fang J.H.Fan Y.Z.Fan C.F Feng l.Feng s.H.Feng Y.l.Feng B.Gao Q.Gao W.Gao M.M.Ge l.s.Geng G.H.Gong Q.B.Gou M.H.Gu Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He J.C.He M.Heller s.l.He Y.He C.Hou D.H.Huang Q.l.Huang W.H.Huang X.T.Huang H.B.Hu s.Hu H.Y.Jia K.Jiang F.Ji C.Jin X.l.Ji K.levochkin E.W.liang Y.F liang Cheng li Cong li F.li H.li H.B.li H.C.li H.M.li J.li K.li W.l.li X.li X.R.li Y.li Z.li Z.li B.liu C.liu D.liu H.D.liu H.liu J.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 J.R.Mao A.Masood X.H.Ma W.Mitthumsiri T.Montaruli Y.C.Nan P.Pattarakijwanich Z.Y.Pei B.Q.Qiao M.Y.Qi D.Ruffolo V.Rulev a.s.iz.l.s.ao O.shchegolev X.D.sheng J.R.shi Y.stenkin V.stepanov Z.B.sun P.H.T.Tam Z.B.Tang W.W.Tian D.D.Volpe C.Wang H.Wang H.G.Wang J.C.Wang l.Y.Wang W.Wang W.Wang X.G.Wang X.Y.Wang X.J.Wang Y.D.Wang Y.J.Wang Y.N.Wang Y.P.Wang Z.Wang Z.H.Wang Z.X.Wang D.M.Wei J.J.Wei T.Wen C.Y.Wu H.R.Wu s.Wu W.X.Wu X.F.Wu G.M.Xiang G.Xiao G.G.Xin Y.Xing R.X.Xu l.Xue D.H.Yan C.W.Yang F.F.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 Q.Yuan Y.H.Yu Z.J.Jiang H.D.Zeng T.X.Zeng W.Zeng Z.K.Zeng M.Zha B.B.Zhang H.M.Zhang H.Y.Zhang J.l.Zhang J.W.Zhang l.Zhang P.F.Zhang P.P.Zhang s.R.Zhang s.s.Zhang X.Zhang X.P.Zhang Yi Zhang Yong Zhang Y.F.g Zhang B.Zhao J.Zhao l.Zhao l.Z.Zhao F.Zheng Y.Zheng J.N.Zhou P.Zhou R.Zhou X.X.Zhou C.G.Zhu F.R.Zhu H.Zhu K.J.Zhu X.Zuo Institute of High Energy Physics Chinese Academy of SciencesBeijing 100049China University of Chinese Academy of sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduShichuanChina University of science and Technology of China 230026 HefeiAnhuiChina Tsinghua University 100084 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 sun Yat-sen University 519000 ZhuhaiGuangdongChina shool of Physics and Technology Guangxi University530004 NanningGuangxiChina Hebei Normal University 050024 ShijiazhuangHebeiChina school of Physics and Engineering Zhengzhou University450001 ZhengzhouHenanChina Nanjing University 210023 NanjingJiangsuChina Key laboratory of Dark Matter and space Astronomy Purple Mountain ObservatoryChinese Academy of Sciences210034 NanjingJiangsuChina Institute of Frontier and Interdisciplinary science Shandong University266237 QingdaoShandongChina shanghai Astronomical Observatory Chinese Academy of Sciences200030 ShanghaiChina school of Physical science and Technology Southwest Jiaotong University610031 ChengduSichuanChina sichuan University 610065 ChengduSichuanChina Key laboratory of Cosmic Rays(Tibet University) Ministry of Education850000 LhasaTibetChina school of physics and technology Wuhan university430072 WuhanChina Yunnan University 650091 KunmingYunnanChina Yunnan Astronomical Observatories Chinese Academy of Sciences650216 KunmingYunnanChina Institute for Nuclear Research Russian Academy of SciencesMoscowRussia Département de Physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde GenéveGenevaSwitzerland Department of Physics Faculty of ScienceMahidol UniversityBangkokThailand Dublin Institute for Advanced studies 31 Fitzwilliam PlaceDublin 2Ireland Max-Planc

The Water Cherenkov Detector Array(WCDA) is a major component of the large High Altitude Air shower Array Observatory(lHAAsO), a new generation cosmic-ray experiment with unprecedented sensitivity, currently under construction. WCDA is aimed at the study of TeV γ-rays. In order to evaluate the prospects of searching for TeV γ-ray sources with WCDA, we present a projection of the one-year sensitivity of WCDA to TeV γ-ray sources from TeVCat using an all-sky approach. Out of 128 TeVCat sources observable by WCDA up to a zenith angle of 45°, we estimate that 42 would be detectable in one year of observations at a median energy of 1 TeV. Most of them are Galactic sources, and the extragalactic sources are Active Galactic Nuclei(AGN).

关键词： TeVγ-ray astronomy observational prospect lHAAsO-WCDA

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The human olfactory system in two proteinopathies: Alzheimer’s and Parkinson’s diseases

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Translational Neurodegeneration 2020年第2期9卷 270-289页

作者： Isabel Ubeda-Bañon Daniel saiz-sanchez Alicia Flores-Cuadrado Ernesto Rioja-Corroto Melania Gonzalez-Rodriguez sandra Villar-Conde Veronica Astillero-lopez Juan Pablo Cabello-de la Rosa Maria Jose Gallardo-Alcañiz Julia Vaamonde-Gamo Fernanda Relea-Calatayud lucia Gonzalez-lopez Alicia Mohedano-Moriano Alberto Rabano Alino Martinez-Marcos Neuroplasticity and Neurodegeneration laboratory Ciudad Real Medical SchoolCRIBUniversity of Castilla-La Mancha13005Ciudad RealSpain Neurology service Ciudad Real General University Hospital13005Ciudad RealSpain Pathology service Ciudad Real General University Hospital13005Ciudad RealSpain Faculty of Health sciences University of Castilla-La ManchaTalavera de la ReinaSpain Neuropathology Department and Tissue Bank CIEN FoundationCarlos III Health InstituteMadridSpain

Alzheimer’s and Parkinson’s diseases are the most prevalent neurodegenerative *** etiologies are idiopathic,and treatments are symptomatic and orientated towards cognitive or motor ***,both are proteinopathies with pathological aggregates(plaques of amyloid-β peptide and neurofibrillary tangles of tau protein in Alzheimer’s disease,and lewy bodies mostly composed of α-synuclein in Parkinson’s disease).These deposits appear in the nervous system in a predictable and accumulative sequence with six neuropathological *** disorders present a long prodromal period,characterized by preclinical signs including ***,the olfactory system,particularly the anterior olfactory nucleus,is initially and preferentially affected by the *** atrophy revealed by magnetic resonance imaging must be complemented by histological analyses to ascertain whether neuronal and/or glial loss or neuropil remodeling are responsible for volumetric *** has been proposed that these proteinopathies could act in a prion-like manner in which a misfolded protein would be able to force native proteins into pathogenic folding(seeding),which then propagates through neurons and glia(spreading).Existing data have been examined to establish why some neuronal populations are vulnerable while others are resistant to pathology and to what extent glia prevent and/or facilitate proteinopathy *** approaches reveal a number of hubs in the olfactory system(anterior olfactory nucleus,olfactory entorhinal cortex and cortical amygdala)that are key interconnectors with the main hubs(the entorhinal–hippocampal–cortical and amygdala–dorsal motor vagal nucleus)of network dysfunction in Alzheimer’s and Parkinson’s diseases.

关键词： α-synuclein Amyloid-β Anterior olfactory nucleus Hyposmia Tau protein

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