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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

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Antineutrino energy spectrum unfolding based on the Daya Bay measurement and its applications

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Chinese Physics C 2021年第7期45卷 1-19页

作者： F.P.An A.B.Balantekin 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 D.Dolzhikov J.Dove M.Dvorak D.A.Dwyer J.P.Gallo M.Gonchar G.h.Gong h.Gong M.Grassi W.Q.Gu J.Y.Guo L.Guo x.h.Guo Y.h.Guo Z.Guo R.W.hackenburg S.hans a M.he K.M.heeger Y.K.heng Y.K.hor Y.B.hsiung B.Z.hu J.R.hu T.hu Z.J.hu h.x.huang J.h.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.Kettel S.Kohn M.Kramer T.J.Langford J.Lee J.h.C.Lee R.T.Lei R.Leitner J.K.C.Leung F.Li h.L.Li J.J.Li Q.J.Li R.h.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.Link26 L.Littenberg B.R.Littlejohn J.C.Liu J.L.Liu J.x.Liu C.Lu h.Q.Lu K.B.Luk B.Z.Ma x.B.Ma x.Y.Ma Y.Q.Ma R.C.Mandujano C.Marshall K.T.McDonald R.D.McKeown Y.Meng J.Napolitano D.Naumov E.Naumova T.M.T.Nguyen J.P.Ochoa-Ricoux A.Olshevskiy 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.Tmej1 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 h.K.xu 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 V.Zavadskyi S.Zeng Y.Zeng L.Zhan C.Zhang F.Y.Zhang h.h.Zhang J.W.Zhang Q.M.Zhang S.Q.Zhang x.T.Zhang Y.M.Zhang Y.x.Zhang Y.Y.Zhang Z.J.Zhang Z.P.Zhang Z.Y.Zhang J.Zhao R.Z.Zhao L.Zhou h.L.Zhuang J.h.Zou Institute of Modern Physics East China University of Science and TechnologyShanghai 200337 University of Wisconsin MadisonWisconsin 53706 Brookhaven National Laboratory UptonNew York 11973 Department of Physics Nnational Taiwan UniversityTaipei Institute of high Energy Physics Beijing 100049 National United University Miao-Li Department of Engineering Physics Tsinghua UniversityBeijing 100048 Shenzhen University Shenzhen 518061 Sun Yat-Sen(Zhongshan)University Guangzhou 510275 North China Electric Power University Beijing 102206 Chinese University of hong Kong Hongkong 999077 Siena College LoudonvilleNew York 12211 Department of Physics and Astronomy University of CaliforniaIrvineCalifornia 92697 University of Science and Technology of China Hefei 230022 Charles University Faculty of Mathematics and PhysicsPrague Joint Institute for Nuclear Research DubnaMoscow Region Department of Physics University of Illinois at Urbana-ChampaignUrbanaIllinois 61801 Lawrence Berkeley National Laboratory BerkeleyCalifornia 94720 Department of Physics Illinois Institute of TechnologyChicagoIllinois 60616 Beijing Normal University Beijing 100875 Department of Nuclear Science and Technology School of Energy and Power EngineeringXi'an Jiaotong UniversityXi'an 710049 Wright Laboratory and Department of Physics Yale UniversityNew HavenConnecticut 06520 China Institute of Atomic Energy Beijing 102413 Shandong University Jinan 250002 Guangxi University No.100 Daxue East RoadNanning 530004 Center for Neutrino Physics Virginia TechBlacksburgVirginia 24061 Institute of Physics NCTUHsinchu Department of Physics University of CincinnatiCincinnatiOhio 45221 Department of Physics College 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 KongPokfulamHongkong 999077 School of Physics Nankai UniversityTianjin 300071 Department o

The prediction of reactor antineutrino spectra will play a crucial role as reactor experiments enter the precision *** positron energy spectrum of 3.5 million antineutrino inverse beta decay reactions observed by the Daya Bay experiment,in combination with the fission rates of fissile isotopes in the reactor,is used to extract the positron energy spectra resulting from the fission of specific *** information can be used to produce a precise,data-based prediction of the antineutrino energy spectrum in other reactor antineutrino experiments with different fission fractions than Daya *** positron energy spectra are unfolded to obtain the antineutrino energy spectra by removing the contribution from detector response with the Wiener-SVD unfolding *** results are obtained with other unfolding methods.A technique to construct a data-based prediction of the reactor antineutrino energy spectrum is proposed and *** the reactor fission fractions,the technique can predict the energy spectrum to a 2%*** addition,we illustrate how to perform a rigorous comparison between the unfolded antineutrino spectrum and a theoretical model prediction that avoids the input model bias of the unfolding method.

关键词： reactor antineutrino energy spectrum Daya Bay application

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Dynamical complexity of Anosov systems driven by a quasi-periodic force

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Science China Mathematics 2025年第1期68卷 89-136页

作者： Wen huang Zeng Lian Kening Lu Department of Mathematics University of Science and Technology of ChinaHefei 230026China School of Mathematics Sichuan UniversityChengdu 610065China

Consider C^(2)Anosov systems on a compact manifold driven by a quasi-periodic *** study their dynamical complexity on various levels from the perspectives of both path-wise dynamics and stochastic *** that these systems are non-wandering(i.e.,every point in the phase space is nonwandering),we prove a set of results:(1)the existence of abundance of random periodic points;(2)a random Livsic theorem;(3)a random Mañé-Bousch-Conze-Guivarc'h lemma;(4)the existence of strong random ***,a concrete example constructed on a 2-dimensional torus is also given to uncover some interesting phenomena of the systems.

关键词： random Anosov systems Anosov system on bers entropy random periodic orbit random horseshoe cohomological equation random Livsic theorem random Bousch-Mañécohomology lemma

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No-go guide for the hubble tension:Late-time or local-scale new physics

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Science China(Physics,Mechanics & Astronomy) 2025年第2期68卷 73-85页

作者： Lu huang Shao-Jiang Wang Wang-Wei Yu CAS Key Laboratory of Theoretical Physics Institute of Theoretical PhysicsChinese Academy of Sciences(CAS)Beijing100190China Asia Pacific Center for Theoretical Physics(APCTP) Pohang37673Korea Max-Planck-Institut für Gravitationsphysik(Albert-Einstein-Institut) HannoverD-30167Germany Leibniz Universität hannover Hannover30167Germany

The standard model of modern cosmology might be cracked by the recent persistent hot debate on the hubble-constant(h_(0))tension,which manifests itself as the sound-horizon(r_(s))tension or absolute-magnitude(M_(B))tension if deeming the origin of the hubble tension from modifying the early or late Universe,*** this study,we achieve a fully model-independent constraint(fitting a model-independent global parameterization to a model-independent inverse distant ladder with a modelindependent high-redshift calibration)on late-time models with strong evidence against homogeneous new physics over theΛ-cold-dark-matter(ΛCDM)*** using this model-independent constraint to calibrate sufficiently local supernovae with corresponding late-time models extrapolated below the homogeneity scale,we find surprisingly that,although both h_(0)tension and MB tension are absent in our local Universe,a combination of h_(0)and M_(B)as the intercept a B of the magnitude-redshift relation exhibits 3~7σtension even for theΛCDM *** aBtension seems to call for local-scale inhomogeneous new physics disguised as local observational systematics.

关键词： hubble constant inverse distance ladder local Universe

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Compound heterozygous mutation of AFG3L2 causes autosomal recessive spinocerebellar ataxia through mitochondrial impairment and MICU1 mediated Ca2+overload

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Science China(Life Sciences) 2025年第2期68卷 484-501页

作者： hongyu Li Qingwen Ma Yan xue Linlin Cai Liwen Bao Lei hong Yitao Zeng Shu-Zhen huang Richard h.Finnell Fanyi Zeng Shanghai Institute of Medical Genetics Shanghai Children’s HospitalShanghai Jiao Tong University School of MedicineShanghai 200040China Department of histo-Embryology Genetics and Developmental BiologyShanghai Jiao Tong University School of MedicineShanghai 200025China NhC Key Laboratory of Medical Embryogenesis and Developmental Molecular Biology Shanghai Key Laboratory of Embryo and Reproduction EngineeringShanghai 200040China Center for Precision Environmental health Baylor College of MedicineHouston 77030USA School of Pharmacy Macao University of Science and TechnologyMacao 999078China

Autosomal recessive spinocerebellar ataxias(SCARs)are one of the most common neurodegenerative diseases characterized by progressive *** SCARs are known to be caused by mutations in multiple genes,there are still many cases that go undiagnosed or are *** this study,we presented a SCAR patient,and identified a probable novel pathogenic mutation(c.1A>G,p.M1V)in the AFG3L2 start *** proband's genotype included heterozygous mutations of the compound AFG3L2(p.[M1V];[R632x](c.[1A>G];[1894.C>T])),which were inherited from the father(c.1A>G,p.M1V)and mother(c.1894C>T,p.R632x).Functional studies performed on hi PSCs(human induced pluripotent stem cells)generated from the patients and hEK293T cells showed that the mutations impair mitochondrial function and the unbalanced expression of AFG3L2 mRNA and protein ***,this novel mutation resulted in the degradation of the protein and the reduction of the stability of the AFG3L2 protein,and MCU(mitochondrial calcium uniporter)complex mediated Ca2+overload.

关键词： AFG3L2 gene autosomal recessive spinocerebellar ataxia mitochondrial impairment Ca2+overload

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Vertical gradients of neutral winds observed by ICON and estimated by the horizontal Wind Model during the geomagnetic storm on August 26−28,2021

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Earth and Planetary Physics 2025年第1期9卷 69-80页

作者： JiaWei Wu Chao xiong YuYang huang YunLiang Zhou Department of Space Physics School of Electronic InformationHubei Luojia LaboratoryWuhan UniversityWuhan 430072China

The Michelson Interferometer for Global high-resolution Thermospheric Imaging(MIGhTI)onboard the Ionospheric Connection Explorer(ICON)satellite offers the opportunity to investigate the altitude profile of thermospheric *** this study,we used the red-line measurements of MIGhTI to compare with the results estimated by horizontal Wind Model 14(hWM14).The data selected included both the geomagnetic quiet period(December 2019 to August 2022)and the geomagnetic storm on August 26-28,*** the geomagnetic quiet period,the estimations of neutral winds from hWM14 showed relatively good agreement with the observations from *** to the ICON observations,near the equator,zonal winds reverse from westward to eastward at around 06:00 local time(LT)at higher altitudes,and the stronger westward winds appear at later LTs at lower *** around 16:00 LT,eastward winds at 300 km reverse to westward,and vertical gradients of zonal winds similar to those at sunrise hours can be *** the middle latitudes,zonal winds reverse about 2-4 h *** winds vary more significantly than zonal winds with seasonal and latitudinal *** to the ICON observations,in the northern low latitudes,vertical reversals of meridional winds are found at 08:00-13:00 LT from 300 to 160 km and at around 18:00 LT from 300 to 200 km during the June *** reversals of meridional winds are found at 04:00-07:00 LT from 300 to 160 km and at 22:00-02:00 LT from 270 to 200 km during the December *** the southern low latitudes,meridional wind reversals occur at 08:00-11:00 LT from 200 to 160 km and at 21:00-02:00 LT from 300 to 200 km during the June *** the December solstice,reversals of the meridional wind appear at 20:00-01:00 LT below 200 km and at 06:00-11:00 LT from 300 to 160 *** the northern middle latitudes,the northward winds are dominant at 08:00-14:00 LT at 230 km during the June *** winds persist until

关键词： horizontal neutral winds vertical gradients Ionospheric Connection Explorer satellite horizontal Wind Model 14 geomagnetic storm

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Thermal effects on wear behavior of additively manufactured NiTi shape memory alloys

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Chinese Journal of Aeronautics 2025年第1期38卷 147-164页

作者： xianghui huang Nan KANG Pei WANG Mohamed EL MANSORI Arts et Metiers Institute of Technology MSMPHESAM UniversitéChâlons-en-Champagne 51006France henan Key Laboratory of high-Performance Carbon Fiber Reinforced Composites Institute of Carbon Matrix CompositesHenan Academy of SciencesZhengzhou 450046China Texas A&M Engineering Experiment Station Institute for Manufacturing SystemsCollege StationTX 77843USA

NiTi alloys fabricated by laser powder bed fusion(LPBF)additive manufacturing technology not only address the compositional instability resulting from complex processes but also solve the challenges of difficult machining of intricate aerospace ***,there are very few reports on the wear behavior of LPBF-NiTi *** the present work,the effects of microstructure and thermal treatment,including heat treatment and frictional heat,on the wear behavior of LPBF-NiTi alloy and 100Cr6 ball were analyzed through a series of tribological experiments with different sliding *** the average sliding speed increases(0.079–0.216 m/s),the wear rate of the as-built and heat-treated samples tends to decrease in the range of 2.69×10^(-3)–0.97×10^(-3)mm^(3)/*** the heat-treated LPBF-NiTi alloy is 46%harder than the as-built alloy is,the latter has a higher toughness(505 MJ/m^(3))and greater transformation strain of SIM(0.097).This leads to a coupling effect of heat treatment and sliding speed on the wear *** addition,the wear track morphologies under different sliding speeds are asymmetric due to the 24% greater acceleration at the far end from the motor and the 2.15 mm deviation between the maximum speed position and the geometric center of the *** wear modes of the as-built and heat-treated samples included adhesive,abrasive and delamination ***,the wear morphologies and dominant wear modes change with the frictionally caused heat release induced by the sliding speed.

关键词： Additive manufacturing Laser powder bed fusion NiTi alloys Wear resistance Sliding speed

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Ultrafast sodium storage of alkylamine molecule tailored MnPS_(3) enabled by quasi-topological intercalation mechanism

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Science China Chemistry 2025年第2期68卷 552-560页

作者： xueyang Tu Ke Fan Baixin Peng Zhuoran Lv Yiran hao Wujie Dong Wei Zhao Zuocheng Wang haitao huang Yuqiang Fang Fuqiang huang State Key Lab of Metal Matrix Composites School of Materials Science and EngineeringShanghai Jiao Tong UniversityShanghai 200240China Zhangjiang Institute for Advanced Study Shanghai Jiao Tong UniversityShanghai 200240China State Key Laboratory of high-Performance Ceramics and Superfine Microstructure Shanghai Institute of CeramicsChinese Academy of SciencesShanghai 200050China Center of Materials Science and Optoelectronics Engineering University of Chinese Academy of SciencesBeijing 100049China Research Institute for Smart Energy The Hong Kong Polytechnic UniversityHong Kong 999077China Jiangxi Far East Battery Co. Ltd.Yichun 330600China

Two-dimensional transition metal trithiophosphates(TMPS_(3),TM=Mn,Fe,Co,etc.)are competitive anode materials for sodium-ion batteries(SIBs)due to their high theoretical capacity(>1,300 mAh g^(−1))but suffer from limited practical capacity(~300 mAh g^(−1))and inferior rate capability caused by sluggish Na+intercalation/deintercalation kinetics and severe structural ***,alkylamine molecules are first proposed as intercalation guests to significantly boost the electrochemical activity and stability of MnPS_(3).Compared to MnPS_(3),C3h9N-MnPS_(3) enlarges the interlayer spacing from 6.48 to 10.23Åand shows a 105 times higher electrical conductivity,which provides fast ion/electron transport and high strain adaptability,realizing a quasi-topological Na+intercalation ***,C3h9N-MnPS_(3) exhibits an ultrahigh reversible capacity of 775 mAh g^(−1) at 0.5 A g^(−1) and superior high-rate cycling stability with~100%capacity retention after 2,500 cycles at 15 A g^(−1),ranking it among the top metal trithiophosphate-based anode materials *** calculations indicate that the improved sodium storage performance of C3h9N-MnPS_(3) results from the reduced bonding energy of P–S bonds and increased adsorption energy of Na^(+).This work is expected to provide an efficient strategy for the design of high-performance layered anode materials for SIBs.

关键词： transition metal trithiophosphates intercalation guest sodium-ion batteries quasi-topological intercalation

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Deep view of composite SNR CTA1 with LhAASO in γ-rays up to 300 TeV

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Science China(Physics,Mechanics & Astronomy) 2025年

作者： Zhen Cao F.Aharonian Axikegu Y.x.Bai Y.W.Bao D.Bastieri x.J.Bi Y.J.Bi W.Bian A.V.Bukevich Q.Cao W.Y.Cao Zhe Cao J.Chang J.F.Chang A.M.Chen E.S.Chen h.x.Chen Liang Chen Lin Chen Long Chen M.J.Chen M.L.Chen Q.h.Chen S.Chen S.h.Chen S.Z.Chen T.L.Chen Y.Chen N.Cheng Y.D.Cheng M.C.Chu M.Y.Cui S.W.Cui x.h.Cui Y.D.Cui B.Z.Dai h.L.Dai Z.G.Dai Danzengluobu x.Q.Dong K.K.Duan J.h.Fan Y.Z.Fan J.Fang J.h.Fang K.Fang C.F.Feng h.Feng L.Feng S.h.Feng x.T.Feng Y.Feng Y.L.Feng S.Gabici B.Gao C.D.Gao Q.Gao W.Gao W.K.Gao M.M.Ge T.T.Ge L.S.Geng G.Giacinti G.h.Gong Q.B.Gou M.h.Gu F.L.Guo J.Guo x.L.Guo Y.Q.Guo Y.Y.Guo Y.A.han O.A.hannuksela M.hasan h.h.he h.N.he J.Y.he Y.he Y.K.hor B.W.hou C.hou x.hou h.B.hu Q.hu S.C.hu C.huang D.h.huang T.Q.huang W.J.huang x.T.huang x.Y.huang Y.huang Y.Y.huang x.L.Ji h.Y.Jia K.Jia h.B.Jiang K.Jiang x.W.Jiang Z.J.Jiang M.Jin M.M.Kang I.Karpikov D.Khangulyan D.Kuleshov K.Kurinov B.B.Li C.M.Li Cheng Li Cong Li D.Li F.Li h.B.Li h.C.Li Jian Li Jie Li K.Li S.D.Li W.L.Li W.L.Li x.R.Li xin Li Y.Z.Li Zhe Li Zhuo Li E.W.Liang Y.F.Liang S.J.Lin B.Liu C.Liu D.Liu D.B.Liu h.Liu h.D.Liu J.Liu J.L.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.Liu Y.N.Liu Q.Luo Y.Luo h.K.Lv B.Q.Ma L.L.Ma x.h.Ma J.R.Mao Z.Min W.Mitthumsiri h.J.Mu Y.C.Nan A.Neronov K.C.Y.Ng L.J.Ou P.Pattarakijwanich Z.Y.Pei J.C.Qi M.Y.Qi B.Q.Qiao J.J.Qin A.Raza D.Ruffolo A.Sáiz M.Saeed D.Semikoz L.Shao O.Shchegolev x.D.Sheng F.W.Shu h.C.Song Yu.V.Stenkin V.Stepanov Y.Su D.x.Sun Q.N.Sun x.N.Sun Z.B.Sun J.Takata P.h.T.Tam Q.W.Tang R.Tang Z.B.Tang W.W.Tian L.h.Wan C.Wang C.B.Wang G.W.Wang h.G.Wang h.h.Wang J.C.Wang Kai Wang Kai Wang L.P.Wang L.Y.Wang P.h.Wang R.Wang W.Wang x.G.Wang x.Y.Wang Y.Wang Y.D.Wang Y.J.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 Q.W.Wu S.Wu x.F.Wu Y.S.Wu S.Q.xi J.xia G.M.xiang D.x.xiao G.xiao Y.L.xin Y.xing D.R.xiong Z.xiong D.L.xu R.F.xu R.x.xu W.L.xu L.xue D.h.Yan J.Z.Yan T.Yan C.W.Yang C.Y.Yang F.Yang F.F.Yang L.L.Yang M.J.Yang R.Z.Yang W.x.Yang Y.h.Yao Z.G.Yao L.Q.Yin N.Yin x.h.You Z.Y.You Y.h Southwest Jiaotong University School of Astronomy and Space Science Nanjing University Center for Astrophysics Guangzhou University Tsung-Dao Lee Institute & School of Physics and Astronomy Shanghai Jiao Tong University Institute for Nuclear Research of Russian Academy of Sciences hebei Normal University University of Science and Technology of China LhAASO Collaboration State Key Laboratory of Particle Detection and Electronics Key Laboratory of Dark Matter and Space Astronomy & Key Laboratory of Radio Astronomy Purple Mountain Observatory Chinese Academy of Sciences Research Center for Astronomical Computing Zhejiang Laboratory Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences School of Physics and Astronomy Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center Yunnan University Key Laboratory of Cosmic Rays (Tibet University) Ministry of Education Department of Physics The Chinese University of hong Kong Key Laboratory of Radio Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences School of Physics and Astronomy (Zhuhai) & School of Physics (Guangzhou) & Sino-French Institute of Nuclear Engineering and Technology (Zhuhai) Sun Yat-sen University Institute of high Energy Physics Institute of Frontier and Interdisciplinary Science Shandong University APC Université Paris Cité CNRS/IN2P3 CEA/IRFU Observatoire de Paris Department of Engineering Physics & Department of Astronomy Tsinghua University School of Physics and Microelectronics Chinese Academy of Sciences Zhengzhou University Yunnan Observatories Chinese Academy of Sciences China Center of Advanced Science and Technology College of Physics Sichuan University School of Physics Peking University Guangxi Key Laboratory for Relativistic Astrophysics School of Physical Science and Technology University of Chinese Academy of Sciences Guangxi University Department of Physics Faculty of Science Mahidol University Moscow Institute

The ultra-high-energy（UhE） gamma-ray source 1LhAASO J0007+7303u is positionally associated with the composite SNR CTA1 that is located at high Galactic Latitude b ≈ 10.5°. This provides a rare opportunity to spatially resolve the component of the pulsar wind nebula（PWN） and supernova remnant（SNR） at UhE. This paper conducted a dedicated data analysis of 1LhAASO J0007+7303u using the data collected from December 2019 to July 2023. This source is well detected with significances of 21σ and 17σ at 8-100 TeV and >100 TeV, respectively. The corresponding extensions are determined to be 0.23°±0.03°and 0.17°±0.03°. The emission is proposed to originate from the relativistic electrons accelerated within the PWN of PSR J0007+7303. The energy spectrum is well described by a power-law with an exponential cutoff function dN/dE =（42.4 ± 4.1）(E/（20 TeV）)-2.31±0.11exp(-E/（110±25 TeV）) TeV-1cm-2s-1in the energy range from 8 to 300 TeV, implying a steady-state parent electron spectrum dNe/dEe∝(Ee/（100 TeV）)-3.13±0.16exp[(-Ee/（373±70 TeV）)2] at energies above ≈ 50 TeV. The cutoff energy of the electron spectrum is roughly equal to the expected current maximum energy of particles accelerated at the PWN terminal shock. Combining the x-ray and gamma-ray emission, the current space-averaged magnetic field can be limited to≈ 4.5 μG. To satisfy the multi-wavelength spectrum and the γ-ray extensions, the transport of relativistic particles within the PWN is likely dominated by the advection process under the free-expansion phase assumption.

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LhAASO detection of very-high-energy γ-ray emission surrounding PSR J0248+6021

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Science China(Physics,Mechanics & Astronomy) 2025年

We report the detection of an extended very-high-energy(VhE) γ-ray source coincident with the location of middle-aged(62.4 kyr) pulsar PSR J0248+6021, by using the LhAASO-WCDA data of live 796 d and LhAASO-KM2A data of live 1216d. A significant excess of γ-ray induced showers is observed both by WCDA in energy bands of 1-25 Te V and KM2A in energy bands of >25 TeV with 7.3σ and 13.5σ, respectively. The best-fit position derived through WCDA data is R.A. = 42.06°± 0.12°and Dec. = 60.24°± 0.13°with an extension of 0.69°±0.15°and that of the KM2A data is R.A.= 42.29°± 0.13°and Dec. =60.38°± 0.07°with an extension of 0.37°±0.07°. No clear extended multiwavelength counterpart of this LhAASO source has been found from the radio band to the GeV band. The most plausible explanation of the VhE γ-ray emission is the inverse Compton process of highly relativistic electrons and positrons injected by the pulsar. These electrons/positrons are hypothesized to be either confined within the pulsar wind nebula or to have already escaped into the interstellar medium, forming a pulsar halo.

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