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Evidence for particle acceleration approaching PeV energies in the W51 complex

science Bulletin 2024年第18期69卷 2833-2841页

作者： LHAASO Collaboration 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.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 L.S.Geng G.Giacinti G.H.Gong Q.B.Gou M.H.Gu F.L.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han 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 D.H.Huang T.Q.Huang W.J.Huang X.T.Huang X.Y.Huang Y.Huang X.L.Ji H.Y.Jia K.Jia K.Jiang X.W.Jiang Z.J.Jiang M.Jin M.M.Kang I.Karpikov 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 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 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.Yu Q.Yuan H.Yue H.D.Zeng T.X.Zeng W.Zeng M.Zha B.B.Zhang F.Zhang H.Zhang 不详 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 ChengduChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institut for Nuclear Physics P.O.Box 103980Heidelberg 69029Germany School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Institute for Nuclear Research of Russian Academy of Sciences Moscow 117312Russia Hebei Normal University Shijiazhuang 050024China University of Science and Technology of China Hefei 230026China State Key Laboratory of Particle Detection and Electronics China Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Research Center for Astronomical Computing Zhejiang LaboratoryHangzhou 311121China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China School of Physics and Astronomy Yunnan UniversityKunming 650091China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Physics and Astronomy(Zhuhai)&School of Physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(Zhuhai) Sun Yat-sen UniversityZhuhai 519000&Guangzhou 510275GuangdongChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China APC UniversitéParis Cité

Theγ-ray emission from the W51 complex is widely acknowledged to be attributed to the interaction between the cosmic rays(CRs)accelerated by the shock of supernova remnant(SNR)W51C and the dense molecular clouds in the adjacent star-forming region,***,the maximum acceleration capability of W51C for CRs remains *** on observations conducted with the Large High Altitude Air Shower Observatory(LHAASO),we report a significant detection ofγrays emanating from the W51 complex,with energies from 2 to 200 *** LHAASO measurements,for the first time,extend theγ-ray emission from the W51 complex beyond 100 TeV and reveal a significant spectrum bending at tens of *** combining the"π^(0)-decay bump"featured data from Fermi-LAT,the broadbandγ-ray spectrum of the W51 region can be well-characterized by a simple pp-collision *** observed spectral bending feature suggests an exponential cutoff at~400 TeV or a power-law break at~200 TeV in the CR proton spectrum,most likely providing the first evidence of SNRs serving as CR accelerators approaching the PeV ***,two young star clusters within W51B could also be theoretically viable to produce the most energeticγrays observed by *** findings strongly support the presence of extreme CR accelerators within the W51 complex and provide new insights into the origin of Galactic CRs.

关键词： UHE c-ray Cosmic rays SNR W51C Star clusters

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Probability vector representation of the Schrödinger equation and Leggett-Garg-type experiments

arXiv

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arXiv 2023年

作者： Hotta, Masahiro Murk, Sebastian Department of Physics Tohoku University Sendai980-8578 Japan Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei10617 Taiwan Quantum Gravity Unit Okinawa Institute of Science and Technology 1919-1 Tancha Onna-son Okinawa904-0495 Japan

Leggett-Garg inequalities place bounds on the temporal correlations of a system based on the principles of macroscopic realism per se and noninvasive measurability. Their conventional formulation relies on the ensemble-averaged products of observables measured at different instants of time. However, a complete description that enables a precise understanding and captures all physically relevant features requires the study of probability distributions associated with noncommuting observables. In this article, we propose a scheme to describe the dynamics of generic N-level quantum systems ("qudits") via a probability vector representation of the Schrödinger equation and define a precise notion of no-signaling in time (NSIT) for the probability distributions of noncommuting observables. This provides a systematic way of identifying the interferences responsible for nonclassical behavior. In addition, we introduce an interference witness measure to quantify violations of NSIT for arbitrary general probabilistic states. For single-qubit systems, we pinpoint the pivotal relation that establishes a connection between the disturbance of observables incurred during a measurement and the resulting NSIT violation. For large-N systems where a manual determination is infeasible, the classification of states as either NSIT-conforming or NSIT-violating may be performed by a machine learning algorithm. We present a proof-of-principle implementation of such an algorithm in which the classifier function is prepared via supervised learning using pseudorandomly generated training data sets composed of states whose corresponding classifications are known a priori. Copyright © 2023, The Authors. All rights reserved.

关键词： Probability distributions

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Quark masses and low-energy constants in the continuum from the tadpole-improved clover ensembles

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Physical Review D 2024年第5期109卷 054507-054507页

作者： Zhi-Cheng Hu Bo-Lun Hu Ji-Hao Wang Ming Gong Guoming Liu Liuming Liu Peng Sun Wei Sun Wei Wang Yi-Bo Yang Dian-Jun Zhao Institute of Modern Physics Chinese Academy of Sciences Lanzhou 730000 China University of Chinese Academy of Sciences School of Physical Sciences Beijing 100049 China CAS Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy of Sciences Beijing 100190 China Institute of High Energy Physics Chinese Academy of Sciences Beijing 100049 China Key Laboratory of Atomic and Subatomic Structure and Quantum Control (MOE) Guangdong Basic Research Center of Excellence for Structure and Fundamental Interactions of Matter Institute of Quantum Matter South China Normal University Guangzhou 510006 China Guangdong-Hong Kong Joint Laboratory of Quantum Matter Guangdong Provincial Key Laboratory of Nuclear Science Southern Nuclear Science Computing Center South China Normal University Guangzhou 510006 China University of Chinese Academy of Sciences Beijing 100049 China. INPAC Shanghai Key Laboratory for Particle Physics and Cosmology Key Laboratory for Particle Astrophysics and Cosmology (MOE) School of Physics and Astronomy Shanghai Jiao Tong University Shanghai 200240 China Southern Center for Nuclear-Science Theory (SCNT) Institute of Modern Physics Chinese Academy of Sciences Huizhou 516000 Guangdong Province China School of Fundamental Physics and Mathematical Sciences Hangzhou Institute for Advanced Study UCAS Hangzhou 310024 China International Centre for Theoretical Physics Asia-Pacific Beijing/Hangzhou 100049 China

We present the light-flavor quark masses and low-energy constants using the 2+1 flavor full-QCD ensembles with stout smeared-clover fermion action and Symanzik gauge action. Both the fermion and gauge actions are tadpole improved self-consistently. The simulations are performed on 11 ensembles at three lattice spacings a∈[0.05,0.11] fm, four spatial sizes L∈[2.5,5.1] fm, seven pion masses mπ∈[135,350] MeV, and several values of the strange quark mass. The quark mass is defined through the partially conserved axial current relation and renormalized to MS¯(2 GeV) through the intermediate regularization independent momentum subtraction scheme. The systematic uncertainty of using the symmetric momentum subtraction scheme is also included. Eventually, we predict mu=2.45(22)(20) MeV, md=4.74(11)(09) MeV, and ms=98.8(2.9)(4.7) MeV with the systematic uncertainties from lattice spacing determination, continuum extrapolation and renormalization constant included. We also obtain the chiral condensate Σ1/3=268.6(3.6)(0.7) MeV and the pion decay constant F=86.6(7)(1.4) MeV in the Nf=2 chiral limit, and the next-to-leading order low-energy constants ℓ3=2.43(54)(05) and ℓ4=4.322(75)(96).

关键词： Lattices Lattice QCD Lattice gauge theory

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Progress Towards a Diffuse Neutrino Search in the Full Livetime of the Askaryan Radio Array 38

Progress Towards a Diffuse Neutrino Search in the Full Livet...

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38th International Cosmic Ray Conference, ICRC 2023

作者： Dasgupta, Paramita Muzio, Marco Stein Ali, S. Allison, P. Archambault, S. Beatty, J.J. Besson, D.Z. Bishop, A. Chen, P. Chen, Y.C. Clark, B.A. Clay, W. Connolly, A. Couberly, K. Cremonesi, L. Cummings, A. Dasgupta, P. Debolt, R. de Kockere, S. de Vries, K.D. Deaconu, C. DuVernois, M.A. Flaherty, J. Friedman, E. Gaior, R. Giri, P. Hanson, J. Harty, N. Hendricks, B. Hoffman, K.D. Huang, J.J. Huang, M.-H. Hughes, K. Ishihara, A. Karle, A. Kelley, J.L. Kim, K.-C. Kim, M.-C. Kravchenko, I. Krebs, R. Kuo, C.Y. Kurusu, K. Latif, U.A. Liu, C.H. Liu, T.C. Luszczak, W. Mase, K. Muzio, M.S. Nam, J. Nichol, R.J. Novikov, A. Nozdrina, A. Oberla, E. Pan, Y. Pfendner, C. Punsuebsay, N. Roth, J. Salcedo-Gomez, A. Seckel, D. Seikh, M.F.H. Shiao, Y.-S. Smith, D. Toscano, S. Torres, J. Touart, J. van Eijndhoven, N. Varner, G.S. Vieregg, A. Wang, M.-Z. Wang, S.-H. Wissel, S.A. Xie, C. Yoshida, S. Young, R. Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Department of Astronomy and Astrophysics Pennsylvania State University University ParkPA16802 United States Department of Physics Pennsylvania State University University ParkPA16802 United States Institute of Gravitation and the Cosmos Center for Multi-Messenger Astrophysics Pennsylvania State University University ParkPA16802 United States Dept. of Physics and Astronomy University of Kansas LawrenceKS66045 United States Dept. of Physics Center for Cosmology and AstroParticle Physics The Ohio State University ColumbusOH43210 United States Dept. of Physics Chiba University Chiba Japan Dept. of Physics University of Wisconsin-Madison MadisonWI53706 United States Dept. of Physics Grad. Inst. of Astrophys. Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei Taiwan Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Physics Enrico Fermi Institue Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Dept. of Physics and Astronomy University College London London United Kingdom Center for Multi-Messenger Astrophysics Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Vrije Universiteit Brussel Brussels Belgium Dept. of Physics and Astronomy University of Nebraska LincolnNE68588 United States Dept. Physics and Astronomy Whittier College WhittierCA90602 United States Dept. of Physics University of Delaware NewarkDE19716 United States Dept. of Energy Engineering National United University Miaoli Taiwan Dept. of Applied Physics National Pingtung University Pingtung County Pingtung City900393 Taiwan Dept. of Physics and Astronomy Denison University GranvilleOH43023 United States National Nano Device Laboratories Hsinchu300 Taiwan Dept. of Physics and Astronomy University of Hawaii ManoaHI9682

The Askaryan Radio Array (ARA) is an in-ice ultrahigh energy (UHE, > 10 PeV) neutrino experiment at the South Pole that aims to detect radio emissions from neutrino-induced particle cascades. ARA has five independent stations which together have collected nearly 24 station-years of data. Each of these stations search for UHE neutrinos by burying in-ice clusters of antennas ∼200 m deep in a roughly cubical lattice with side length ∼15 m. Additionally, the fifth ARA station (A5) has a beamforming trigger, referred to as the Phased Array (PA), consisting of a trigger array of 7 tightly packed vertically-polarized antennas. In this proceeding, we will present a neutrino search with the data of this "hybrid" station, emphasizing its capabilities for improved analysis efficiencies, background rejection, and neutrino vertex reconstruction. This is enabled by combining the closely packed trigger antennas with the long-baselines of the outrigger antennas. We will also place the A5 analysis into the context of the broader five station analysis program, including efforts to characterize and calibrate the detector, model and constrain backgrounds, and reject noise across the entire array. We anticipate this full neutrino search to set world-leading limits above 100 PeV, and inform the next generation of neutrino detection experiments. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Neutrons

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Light cone distribution amplitude for the Λ baryon from lattice QCD

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Physical Review D 2025年第3期111卷 034510-034510页

作者： Min-Huan Chu Haoyang Bai Jun Hua Jian Liang Xiangdong Ji Andreas Schäfer Yushan Su Wei Wang Xiaonu Xiong INPAC Key Laboratory for Particle Astrophysics and Cosmology (MOE) Shanghai Key Laboratory for Particle Physics and Cosmology School of Physics and Astronomy Shanghai Jiao Tong University Shanghai 200240 China Yang Yuanqing Scientific Computering Center Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai 200240 China Faculty of Physics Adam Mickiewicz University ulica Uniwersytetu Poznańskiego 2 61-614 Poznań Poland Institute of High Energy Physics CAS Beijing 100049 China School of Physics University of Chinese Academy of Sciences Beijing 100049 China Key Laboratory of Atomic and Subatomic Structure and Quantum Control (MOE) Guangdong Basic Research Center of Excellence for Structure and Fundamental Interactions of Matter Institute of Quantum Matter South China Normal University Guangzhou 510006 China Guangdong-Hong Kong Joint Laboratory of Quantum Matter Guangdong Provincial Key Laboratory of Nuclear Science Southern Nuclear Science Computing Center South China Normal University Guangzhou 510006 China Department of Physics University of Maryland College Park Maryland 20742 USA Institut für Theoretische Physik Universität Regensburg D-93040 Regensburg Germany Southern Center for Nuclear-Science Theory (SCNT) Institute of Modern Physics Chinese Academy of Sciences Huizhou 516000 Guangdong Province China School of Physics Central South University Changsha 418003 China

We calculate the leading-twist light cone distribution amplitudes of the Λ(uds) baryon using lattice QCD methods within the framework of large-momentum effective theory. Our numerical computations are carried out with Nf=2+1 stout smeared clover fermions and a Symanzik gauge action on a lattice with spacing a=0.077 fm and a pion mass of 303 MeV. To approach the large-momentum region, we simulate the equal-time correlations with the hadron momentum Pz={2.52,3.02,3.52} GeV. We investigate the analytic properties of the baryon quasidistribution amplitude in coordinate space and validate them through our lattice calculations. After renormalization and extrapolation, we present results for the three-dimensional distribution in momentum fractions of the two light quarks. Based on these findings, we briefly discuss the phenomenological impact on weak decays of Λb and outline potential systematic uncertainties that can be improved in the future. This work lays the theoretical foundation for accessing baryon light cone distribution amplitudes from lattice QCD.

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Improvement on the Linearity Response of PandaX-4T with new Photomultiplier Tubes Bases

arXiv

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arXiv 2023年

作者： Luo, Lingyin Fang, Deqing Han, Ke Huang, Di Shang, Xiaofeng Wang, Anqing Wang, Qiuhong Wang, Shaobo Wang, Siguang Xiao, Xiang Yan, Binbin Yan, Xiyu School of Physics State Key Laboratory of Nuclear Physics and Technology Peking University Beijing100871 China Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai200240 China Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China INPAC School of Physics and Astronomy Shanghai Jiao Tong University Shanghai Laboratory for Particle Physics and Cosmology Shanghai200240 China Research Center for Particle Science and Technology Institute of Frontier and Interdisciplinary Science Shandong University Shandong Qingdao266237 China Key Laboratory of Particle Physics and Particle Irradiation of Ministry of Education Shandong University Shandong Qingdao266237 China SJTU Paris Elite Institute of Technology Shanghai Jiao Tong University Shanghai200240 China School of Physics Sun Yat-Sen University Guangzhou510275 China Institute of Modern Physics Fudan University Shanghai200433 China School of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 China

With the expanding reach of physics, xenon-based detectors such as PandaX-4T in the China Jinping Underground Laboratory aim to cover an energy range from sub-keV to multiMeV. A linear response of the photomultiplier tubes (PMTs) is required for both scintillation and electroluminescence signals. Through a dedicated bench test, we investigated the cause of the nonlinear response in the Hamamatsu R11410-23 PMTs used in PandaX-4T. The saturation and suppression of the PMT waveform observed during the commissioning of PandaX-4T were caused by the high-voltage divider base. The bench test data validated the de-saturation algorithm used in the PandaX-4T data analysis. We also confirmed the improvement in linearity of a new PMT base design with three more low radioactivity capacitors at later dynodes, which will be used to upgrade the PMT readout system in PandaX-4T. Copyright © 2023, The Authors. All rights reserved.

关键词： Photomultipliers

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Exploring the baryonic effect signature in the Hyper Suprime-Cam Year 3 cosmic shear two-point correlations on small scales: The S8 tension remains present

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Physical Review D 2025年第6期111卷 063509-063509页

作者： Ryo Terasawa Xiangchong Li Masahiro Takada Takahiro Nishimichi Satoshi Tanaka Sunao Sugiyama Toshiki Kurita Tianqing Zhang Masato Shirasaki Kavli Institute for the Physics and Mathematics of the Universe (WPI) The University of Tokyo Institutes for Advanced Study (UTIAS) The University of Tokyo Chiba 277-8583 Japan Department of Physics University of Tokyo Bunkyo Tokyo 113-0031 Japan Center for Data-Driven Discovery (CD3) Kavli IPMU (WPI) UTIAS The University of Tokyo Kashiwa Chiba 277-8583 Japan McWilliams Center for Cosmology Department of Physics Carnegie Mellon University 5000 Forbes Avenue Pittsburgh Pennsylvania 15213 USA Brookhaven National Laboratory Building 510 Upton New York 11973 USA Department of Astrophysics and Atmospheric Sciences Faculty of Science Kyoto Sangyo University Motoyama Kamigamo Kita-ku Kyoto 603-8555 Japan Center for Gravitational Physics and Quantum Information Yukawa Institute for Theoretical Physics Kyoto University Kyoto 606-8502 Japan Center for Particle Cosmology Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA Max Planck Institute für Astrophysik Karl-Schwarzschild-Straße 1 85748 Garching Germany National Astronomical Observatory of Japan National Institutes of Natural Sciences Mitaka Tokyo 181-8588 Japan The Institute of Statistical Mathematics Tachikawa Tokyo 190-8562 Japan

The baryonic feedback effect is considered as a possible solution to the so-called S8 tension indicated in cosmic shear cosmology. The baryonic effect is more significant on smaller scales, and it affects the cosmic shear two-point correlation functions (2PCFs) with different scale and redshift dependencies from those of the cosmological parameters. In this paper, we use the Hyper Suprime-Cam Year 3 (HSC-Y3) data to measure the cosmic shear 2PCFs (ξ±) down to 0.28 arcminutes, taking full advantage of the high number density of source galaxies in the deep HSC data, to explore a possible signature of the baryonic effect. While the published HSC analysis used the cosmic shear 2PCFs on the angular scales that are sensitive to the matter power spectrum at k≲1 h Mpc−1, the smaller-scale HSC cosmic shear signal allows us to probe the signature of the matter power spectrum up to k≃20 h Mpc−1. Using the accurate emulator of the nonlinear matter power spectrum, darkemulator2, we show that the dark-matter-only model can provide an acceptable fit to the HSC-Y3 2PCFs down to the smallest scales. In other words, we do not find any clear signature of the baryonic effects, or we do not find a systematic shift in the S8 value with the inclusion of the smaller-scale information as would be expected if the baryonic effect were significant. Alternatively, we use a flexible six-parameter model of the baryonic effects, which can lead to both enhancement and suppression in the matter power spectrum compared to the dark-matter-only model, to perform the parameter inference of the HSC-Y3 2PCFs. We find that the small-scale HSC data allow only a fractional suppression of up to 5% in the matter power spectrum at k∼1 h Mpc−1, which is not sufficient to reconcile the S8 tension. Finally, we discuss that ξ− on scales smaller than a few arcminutes can be used to monitor characteristic features caused by the baryonic effect if present, while ξ± with appropriate scale cuts can be used to constra

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A search for the ultra high energy neutrinos with the low threshold phased array trigger system of the Askaryan Radio Array 10

A search for the ultra high energy neutrinos with the low th...

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10th International Workshop on Acoustic and Radio EeV Neutrino Detection Activities, ARENA 2024

作者： Dasgupta, Paramita Ali, S. Allison, P. Archambault, S. Beatty, J.J. Besson, D.Z. Bishop, A. Chen, P. Chen, Y.C. Chen, Y.-C. Clark, B.A. Connolly, A. Couberly, K. Cremonesi, L. Cummings, A. Dasgupta, P. Debolt, R. de Kockere, S. de Vries, K.D. Deaconu, C. DuVernois, M.A. Flaherty, J. Friedman, E. Gaior, R. Giri, P. Hanson, J. Harty, N. Hoffman, K.D. Huang, M.H. Hughes, K. Ishihara, A. Karle, A. Kelley, J.L. Kim, K.-C. Kim, M.-C. Kravchenko, I. Krebs, R. Kuo, C.Y. Kurusu, K. Latif, U.A. Liu, C.H. Liu, T.C. Luszczak, W. Mase, K. Muzio, M.S. Nam, J. Nichol, R.J. Novikov, A. Nozdrina, A. Oberla, E. Pan, Y. Pfendner, C. Punsuebsay, N. Roth, J. Salcedo-Gomez, A. Seckel, D. Seikh, M.F.H. Shiao, Y.-S. Su, S.C. Toscano, S. Torres, J. Touart, J. van Eijndhoven, N. Varner, G.S. Vieregg, A. Wang, M.-Z. Wang, S.-H. Wissel, S.A. Xie, C. Yoshida, S. Young, R. Dept. of Physics Center for Cosmology and AstroParticle Physics The Ohio State University ColumbusOH43210 United States Dept. of Physics and Astronomy University of Kansas LawrenceKS66045 United States Dept. of Physics Chiba University Chiba Japan Dept. of Physics University of Wisconsin-Madison MadisonWI53706 United States Dept. of Physics Grad. Inst. of Astrophys. Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei Taiwan Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Physics and Astronomy University College London London United Kingdom Center for Multi-Messenger Astrophysics Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Dept. of Physics Pennsylvania State University University ParkPA16802 United States Dept. of Astronomy and Astrophysics Pennsylvania State University University ParkPA16802 United States Vrije Universiteit Brussel Brussels Belgium Dept. of Physics Enrico Fermi Institue Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Dept. of Physics and Astronomy University of Nebraska LincolnNE68588 United States Dept. Physics and Astronomy Whittier College WhittierCA90602 United States Dept. of Physics University of Delaware NewarkDE19716 United States Dept. of Energy Engineering National United University Miaoli Taiwan Dept. of Applied Physics National Pingtung University Pingtung County Pingtung City900393 Taiwan Dept. of Physics and Astronomy Denison University GranvilleOH43023 United States National Nano Device Laboratories Hsinchu300 Taiwan Universite Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium Dept. of Physics and Astronomy University of Hawaii ManoaHI96822 United States

The Askaryan Radio Array (ARA) is an in-ice ultra high energy (UHE, > 10 PeV) neutrino experiment at the South Pole that aims to detect UHE neutrino-induced radio emission in ice. ARA consists of five independent stations each consisting of a cubical lattice of in-ice antenna clusters with a side length of ∼10 m buried at ∼200 m below the ice surface. The fifth station of ARA (A5) is special as this station has an additional central string, the phased array (PA), which provides an interferometric trigger that enables ARA to trigger on weak signals that are otherwise buried in noise. Leveraging the low threshold phased array trigger, ARA was the first radio neutrino experiment to demonstrate significant improvement in sensitivity to weak signals. In this contribution, we present initial results from a neutrino search combining information from both the traditional station antennas and the phased array antennas of the A5 station. We show the improved vertex reconstruction achieved with this approach, and leveraging this improvement, we expect to enhance the analysis efficiency beyond what has been achieved previously by ARA. This analysis is the paradigmatic representation of future neutrino searches with the next generation of in-ice neutrino experiments. © Copyright owned by the author(s).

关键词： Antenna phased arrays

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Developing New Analysis Tools for Near Surface Radio-based Neutrino Detectors 38

Developing New Analysis Tools for Near Surface Radio-based N...

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38th International Cosmic Ray Conference, ICRC 2023

作者： Barwick, Steven W. Anker, A. Baldi, P. Barwick, S.W. Beise, J. Besson, D.Z. Chen, P. Gaswint, G. Glaser, C. Hallgren, A. Hanson, J.C. Klein, S.R. Kleinfelder, S.A. Lahmann, R. Liu, J. Nam, J. Nelles, A. Paul, M.P. Persichilli, C. Plaisier, I. Rice-Smith, R. Tatar, J. Terveer, K. Wang, S.-H. Welling, C. Zhao, L. University of California Department of Physics and Astronomy IrvineCA United States Department of Physics and Astronomy University of California IrvineCA92697 United States Department of Information and Computer Science University of California IrvineCA92697 United States Uppsala University Department of Physics and Astronomy UppsalaSE-752 37 Sweden Department of Physics and Astronomy University of Kansas LawrenceKS66045 United States Department of Physics Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei10617 Taiwan Whittier College Department of Physics WhittierCA90602 United States Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Electrical Engineering and Computer Science University of California IrvineCA92697 United States ECAP Friedrich-Alexander-Universität Erlangen-Nürnberg Erlangen91058 Germany Deutsches Elektronen-Synchrotron DESY Zeuthen15738 Germany Research Cyberinfrastructure Center University of California IrvineCA92697 United States The William H. Miller III Department of Physics & Astronomy Johns Hopkins University BaltimoreMD21218 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States

The ARIANNA experiment is an Askaryan radio detector designed to measure high-energy neutrino induced cascades within the Antarctic ice. Ultra-high-energy neutrinos above 1016 eV have an extremely low flux, so experimental data captured at trigger level need to be classified correctly to retain as much neutrino signal as possible. We first describe two new physics-based neutrino selection methods, or "cuts", (the updown and dipole cut) that extend the previously published analysis to a specialized ARIANNA station with 8 antenna channels, which is double the number used in the prior analysis. The new cuts produce a neutrino efficiency of > 95% per station-year of operation, while rejecting 99.93% of the background (corresponding to 53 remaining experimental background events). When the new cuts are combined with a previously developed cut using neutrino waveform templates, all background is removed at no change of efficiency. In addition, the neutrino efficiency is extrapolated to 1,000 station-years of operation, obtaining 91%. This work then introduces a new selection method (the deep learning cut) to augment the identification of neutrino events by using deep learning methods and compares the efficiency to the physics-based analysis. The deep learning cut gives 99% signal efficiency per station-year of operation while rejecting 99.997% of the background (corresponding to 2 remaining experimental background events), which are subsequently removed by the waveform template cut at no significant change in efficiency. The results of the deep learning cut were verified using measured cosmic rays which shows that the simulations do not introduce artifacts with respect to experimental data. The data driven results in this paper demonstrate that the background rejection and signal efficiency of near surface antennas meets the requirements of a large scale future array, as considered in baseline design of the radio component of IceCube-Gen2. © Copyright owned by the author(

关键词： Cosmic rays

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The Cosmological Dynamics of String Theory Axion Strings

arXiv

引用

arXiv 2023年

作者： Benabou, Joshua N. Bonnefoy, Quentin Buschmann, Malte Kumar, Soubhik Safdi, Benjamin R. Berkeley Center for Theoretical Physics University of California BerkeleyCA94720 United States Theoretical Physics Group Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics Princeton University PrincetonNJ08544 United States GRAPPA Institute Institute for Theoretical Physics Amsterdam University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands Center for Cosmology and Particle Physics Department of Physics New York University New YorkNY10003 United States

The quantum chromodynamics (QCD) axion may solve the strong CP problem and explain the dark matter (DM) abundance of our Universe. The axion was originally proposed to arise as the pseudo-Nambu Goldstone boson of global U(1)PQ Peccei-Quinn (PQ) symmetry breaking, but axions also arise generically in string theory as zero modes of higher-dimensional gauge fields. In this work we show that string theory axions behave fundamentally differently from field theory axions in the early Universe. Field theory axions may form axion strings if the PQ phase transition takes place after inflation. In contrast, we show that string theory axions do not generically form axion strings. In special inflationary paradigms, such as D-brane inflation, string theory axion strings may form;however, their tension is parametrically larger than that of field theory axion strings. We then show that such QCD axion strings overproduce the DM abundance for all allowed QCD axion masses and are thus ruled out, except in scenarios with large warping. A loop-hole to this conclusion arises in the axiverse, where an axion string could be composed of multiple different axion mass eigenstates;a heavier eigenstate could collapse the network earlier, allowing for the QCD axion to produce the correct DM abundance and also generating observable gravitational wave signals. Copyright © 2023, The Authors. All rights reserved.

关键词： String theory

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