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arXiv 2024年

作者： Xu, Gui-Sheng Jain, Mudit Zhou, Xiang-Fa Guo, Guang-Can Amin, Mustafa A. Pu, Han Zhou, Zheng-Wei CAS Key Lab of Quantum Information University of Science and Technology of China Hefei230026 China Synergetic Innovation Center of Quantum Information and Quantum Physics University of Science and Technology of China Hefei230026 China Hefei National Laboratory Hefei230088 China Department of Physics and Astronomy Rice University HoustonTX77251 United States Theoretical Particle Physics and Cosmology King's College London Strand LondonWC2R 2LS United Kingdom

Artificial monopoles have been engineered in various systems, yet there has been no systematic study of the singular vector potentials associated with the monopole field. We show that the Dirac string, the line singularity of the vector potential, can be engineered, manipulated, and made manifest in a spinor atomic condensate. We elucidate the connection among spin, orbital degrees of freedom, and the artificial gauge, and show that there exists a mapping between the vortex filament and the Dirac string. We also devise a proposal where preparing initial spin states with relevant symmetries can result in different vortex patterns, revealing an underlying correspondence between the internal spin states and the spherical vortex structures. Such a mapping also leads to a new way of constructing spherical Landau levels, and monopole harmonics. Our observation provides insights into the behavior of quantum matter possessing internal symmetries in curved spaces. © 2024, CC BY.

关键词： Mapping

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Measurement and interpretation of same-sign W boson pair production in association with two jets in pp collisions at (Formula presented.) TeV with the ATLAS detector

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Journal of High Energy physics 2024年第4期2024卷 1-61页

作者： Aad, G. Abbott, B. Abeling, K. Abicht, N.J. Abidi, S.H. Aboulhorma, A. Abramowicz, H. Abreu, H. Abulaiti, Y. Abusleme Hoffman, A.C. Acharya, B.S. Adam Bourdarios, C. Adamczyk, L. Adamek, L. Addepalli, S.V. Addison, M.J. Adelman, J. Adiguzel, A. Adye, T. Affolder, A.A. Afik, Y. Agaras, M.N. Agarwala, J. Aggarwal, A. Agheorghiesei, C. Ahmad, A. Ahmadov, F. Ahmed, W.S. Ahuja, S. Ai, X. Aielli, G. Aikot, A. Ait Tamlihat, M. Aitbenchikh, B. Aizenberg, I. Akbiyik, M. Åkesson, T.P.A. Akimov, A.V. Akiyama, D. Akolkar, N.N. Al Khoury, K. Alberghi, G.L. Albert, J. Albicocco, P. Albouy, G.L. Alderweireldt, S. Aleksa, M. Aleksandrov, I.N. Alexa, C. Alexopoulos, T. Alfonsi, F. Algren, M. Alhroob, M. Ali, B. Ali, H.M.J. Ali, S. Alibocus, S.W. Aliev, M. Alimonti, G. Alkakhi, W. Allaire, C. Allbrooke, B.M.M. Allen, J.F. Allendes Flores, C.A. Allport, P.P. Aloisio, A. Alonso, F. Alpigiani, C. Alvarez Estevez, M. Alvarez Fernandez, A. Alves Cardoso, M. Alviggi, M.G. Aly, M. Amaral Coutinho, Y. Ambler, A. Amelung, C. Amerl, M. Ames, C.G. Amidei, D. Amor Dos Santos, S.P. Amos, K.R. Ananiev, V. Anastopoulos, C. Andeen, T. Anders, J.K. Andrean, S.Y. Andreazza, A. Angelidakis, S. Angerami, A. Anisenkov, A.V. Annovi, A. Antel, C. Anthony, M.T. Antipov, E. Antonelli, M. Anulli, F. Aoki, M. Aoki, T. Aparisi Pozo, J.A. Aparo, M.A. Aperio Bella, L. Appelt, C. Apyan, A. Aranzabal, N. Arcangeletti, C. Arce, A.T.H. Arena, E. Arguin, J.-F. Argyropoulos, S. Arling, J.-H. Arnaez, O. Arnold, H. Artoni, G. Asada, H. Asai, K. Asai, S. Asbah, N.A. Assamagan, K. Astalos, R. Atashi, S. Atkin, R.J. Atkinson, M. Atmani, H. Atmasiddha, P.A. Augsten, K. Auricchio, S. Auriol, A.D. Austrup, V.A. Avolio, G. Axiotis, K. Azuelos, G. Babal, D. Bachacou, H. Bachas, K. Bachiu, A. Backman, F. Badea, A. Bagnaia, P. Bahmani, M. Bailey, A.J. Bailey, V.R. Baines, J.T. Baines, L. Bakalis, C. Baker, O.K. Bakos, E. Bakshi Gupta, D. Balakrishnan, V. Balasubramanian, R. Baldin, E.M. Balek, P. Ballabene, E. Balli, F. Baltes, L.M. Balunas, W.K. Balz, J. Banas, E. Bandieramont Department of Physics University of Adelaide Department of Physics University of Alberta Department of Physics Ankara University Division of Physics TOBB University of Economics and Technology LAPP Université Savoie Mont Blanc CNRS/IN2P3 APC Université Paris Cité CNRS/IN2P3 High Energy Physics Division Argonne National Laboratory Department of Physics University of Arizona Department of Physics University of Texas at Arlington Physics Department National and Kapodistrian University of Athens Physics Department National Technical University of Athens Department of Physics University of Texas at Austin Institute of Physics Azerbaijan Academy of Sciences Institut de Física d’Altes Energies (IFAE) Barcelona Institute of Science and Technology Institute of High Energy Physics Chinese Academy of Sciences Physics Department Tsinghua University Department of Physics Nanjing University School of Science Shenzhen Campus of Sun Yat-sen University University of Chinese Academy of Science (UCAS) Institute of Physics University of Belgrade Department for Physics and Technology University of Bergen Physics Division Lawrence Berkeley National Laboratory University of California Institut für Physik Humboldt Universität zu Berlin Albert Einstein Center for Fundamental Physics and Laboratory for High Energy Physics University of Bern School of Physics and Astronomy University of Birmingham Department of Physics Bogazici University Department of Physics Engineering Gaziantep University Department of Physics Istanbul University Facultad de Ciencias y Centro de Investigaciónes Universidad Antonio Nariño Departamento de Física Universidad Nacional de Colombia Dipartimento di Fisica e Astronomia A. Righi Università di Bologna INFN Sezione di Bologna Physikalisches Institut Universität Bonn Department of Physics Boston University Department of Physics Brandeis University Transilvania University of Brasov Horia Hulubei National Institute of Physics and Nuclear Engineering Department of Physics Alexandru

This paper presents the measurement of fiducial and differential cross sections for both the inclusive and electroweak production of a same-sign W-boson pair in association with two jets (W^±W^±jj) using 139 fb⁻¹ of proton-proton collision data recorded at a centre-of-mass energy of s = 13 TeV by the ATLAS detector at the Large Hadron Collider. The analysis is performed by selecting two same-charge leptons, electron or muon, and at least two jets with large invariant mass and a large rapidity difference. The measured fiducial cross sections for electroweak and inclusive W^±W^±jj production are 2.92 ± 0.22 (stat.) ± 0.19 (syst.) fb and 3.38 ± 0.22 (stat.) ± 0.19 (syst.) fb, respectively, in agreement with Standard Model predictions. The measurements are used to constrain anomalous quartic gauge couplings by extracting 95% confidence level intervals on dimension-8 operators. A search for doubly charged Higgs bosons H^±± that are produced in vector-boson fusion processes and decay into a same-sign W boson pair is performed. The largest deviation from the Standard Model occurs for an H^±± mass near 450 GeV, with a global significance of 2.5 standard deviations. © The Author(s) 2024.

关键词： Hadron-Hadron Scattering Vector Boson Production

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ARA-Next: a new DAQ and trigger architecture for the Askaryan Radio Array 10

ARA-Next: a new DAQ and trigger architecture for the Askarya...

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

作者： Giri, Pawan Kravchenko, Ilya Allison, Patrick Connolly, Amy L. 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. University of Nebraska - Lincoln LincolnNE United States The Ohio State University ColumbusOH 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 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) experiment aims to detect ultra-high-energy cosmic neutrinos (>10 PeV) using radio detection techniques. To enhance ARA’s capabilities, a new RFSoC-based DAQ, ARA-Next, is in the early stages of development. This advanced system will facilitate the creation of sophisticated triggers, including a novel multi-trigger approach, similar to those used in collider experiments. Our approach involves crafting and implementing innovative triggers for ARA’s new DAQ, such as identifying double pulses from potential in-ice neutrino interactions, utilizing templates for atmospheric cosmic ray signals, optimizing triggers for astrophysical neutrino sources, correlating special events between ARA and IceCube, and discerning anthropogenic events using directional information. These trigger designs aim to lower thresholds and enhance ARA’s detector sensitivity. Overall, this upgrade will not only enhance ARA’s capabilities but also contribute to the technological advancements necessary for future experiments of this nature. © Copyright owned by the author(s).

关键词： Cosmic rays

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Constraining ultralight ALP dark matter in light of cosmic birefringence

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Physical Review D 2024年第10期110卷 103525-103525页

作者： Dongdong Zhang Elisa G. M. Ferreira Ippei Obata Toshiya Namikawa Department of Astronomy School of Physical Sciences University of Science and Technology of China Hefei Anhui 230026 China School of Astronomy and Space Science University of Science and Technology of China Hefei Anhui 230026 China CAS Key Laboratory for Researches in Galaxies and Cosmology University of Science and Technology of China Hefei Anhui 230026 China Kavli Institute for the Physics and Mathematics of the Universe (WPI) UTIAS The University of Tokyo Chiba 277-8583 Japan Center for Data-Driven Discovery Kavli Institute for the Physics and Mathematics of the Universe (WPI) UTIAS The University of Tokyo Chiba 277-8583 Japan

Cosmic birefringence, the observed rotation of the polarization plane of the cosmic microwave background (CMB), serves as a compelling probe for parity-violating physics beyond the Standard Model. This study explores the potential of ultralight axion-like particle (ALP) dark matter to explain the observed cosmic birefringence in the CMB. We focus on the previously understudied mass range of 10−25 to 10−23 eV, where ALPs start to undergo nonlinear clustering in the late Universe. Our analysis incorporates recent cosmological constraints and considers the washout effect on CMB polarization. We find that for models with ALP masses 10−25 eV≲mϕ≲10−23 eV and birefringence arising from late ALP clustering, the upper limit on the ALP-photon coupling constant, imposed by the washout effect, is stringently lower than the coupling required to account for the observed static cosmic birefringence signal. This discrepancy persists regardless of the ALP fraction in dark matter. Furthermore, considering that ALPs with masses mϕ≳10−23 eV cannot explain static birefringence due to their rapid field oscillations, our results indicate that all ALP dark matter candidates capable of nonlinear clustering in the late Universe and thus contributing mainly to the rotation angle of polarized photons are incompatible with explaining the static cosmic birefringence signal observed in Planck and WMAP data.

关键词： Cosmic microwave background particle dark matter

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Confining Strings and Glueballs in ZN Gauge Theories

arXiv

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arXiv 2023年

作者： Athenodorou, Andreas Dubovsky, Sergei Luo, Conghuan Teper, Michael Computation-based Science and Technology Research Center The Cyprus Institute Cyprus Center for Cosmology and Particle Physics Department of Physics New York University New YorkNY10003 United States Rudolf Peierls Centre for Theoretical Physics University of Oxford Parks Road OxfordOX1 3PU United Kingdom All Souls College University of Oxford High Street OxfordOX1 4AL United Kingdom

Effective string theory has shown its universal power in the prediction of the spectrum of low-lying excited states of confining strings. Here we study confining flux tubes in ZN gauge theories. For the N = 2 theory, which corresponds to the 3d Ising gauge model, we compute the spectrum of low-lying excitations of confining strings and show that it agrees with the universal Nambu–Goto predictions except for an additional massive scalar resonance. This resonance, however, turns out to be a bulk glueball mixing with the flux tube excitations rather than a genuine string worldsheet state. In general ZN gauge theories (dual to clock spin models), we observe a continuous phase transition for N ≥ 4, while for N > 5 it is governed by the O(2) universality class. The critical behavior of the string tension and mass gap is verified to be described by a dangerously irrelevant operator. At large N the glueball spectrum is expected to approach the spectrum of U(1) gauge theory, which is confirmed by our lattice data. © 2023, CC BY.

关键词： Lattice theory

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Lens Modeling of STRIDES Strongly Lensed Quasars using Neural Posterior Estimation

arXiv

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arXiv 2024年

作者： Erickson, Sydney Wagner-Carena, Sebastian Marshall, Phil Millon, Martin Birrer, Simon Roodman, Aaron Schmidt, Thomas Treu, Tommaso Schuldt, Stefan Shajib, Anowar Venkatraman, Padma Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University United States SLAC National Accelerator Laboratory United States Center for Data Science New York University United States Center for Computational Astrophysics Flatiron Institute United States Department of Physics and Astronomy Stony Brook University United States Department of Physics and Astronomy University of California Los Angeles United States Dipartimento di Fisica Universita degli Studi di Milano Italy NAF IASF Milano Italy Kavli Institute for Cosmological Physics University of Chicago United States Department of Astronomy and Astrophysics University of Chicago United States Department of Astronomy University of Illinois Urbana-Champaign United States

Strongly lensed quasars can be used to constrain cosmological parameters through time-delay cosmography. Models of the lens masses are a necessary component of this analysis. To enable time-delay cosmography from a sample of O(103) lenses, which will soon become available from surveys like the Rubin Observatory’s Legacy Survey of Space and Time (LSST) and the Euclid Wide Survey, we require fast and standardizable modeling techniques. To address this need, we apply neural posterior estimation (NPE) for modeling galaxy-scale strongly lensed quasars from the Strong Lensing Insights into the Dark Energy Survey (STRIDES) sample. NPE brings two advantages: speed and the ability to implicitly marginalize over nuisance parameters. We extend this method by employing sequential NPE to increase precision of mass model posteriors. We then fold individual lens models into a hierarchical Bayesian inference to recover the population distribution of lens mass parameters, accounting for out-of-distribution shift. After verifying our method using simulated analogs of the STRIDES lens sample, we apply our method to 14 Hubble Space Telescope single-filter observations. We find the population mean of the power-law elliptical mass distribution slope, γlens, to be Mγlens = 2.13 ± 0.06. Our result represents the first population-level constraint for these systems. This population-level inference from fully automated modeling is an important stepping stone towards cosmological inference with large samples of strongly lensed quasars. © 2024, CC BY.

关键词： Dark energy

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Search for Light Dark Matter with Ionization Signals in the PandaX-4T Experiment

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Physical Review Letters 2023年第26期130卷 261001-261001页

作者： Shuaijie Li Mengmeng Wu Abdusalam Abdukerim Zihao Bo Wei Chen Xun Chen Yunhua Chen Chen Cheng Zhaokan Cheng Xiangyi Cui Yingjie Fan Deqing Fang Changbo Fu Mengting Fu Lisheng Geng Karl Giboni Linhui Gu Xuyuan Guo Chencheng Han Ke Han Changda He Jinrong He Di Huang Yanlin Huang Zhou Huang Ruquan Hou Xiangdong Ji Yonglin Ju Chenxiang Li Jiafu Li Mingchuan Li Shu Li Qing Lin Jianglai Liu Xiaoying Lu Lingyin Luo Yunyang Luo Wenbo Ma Yugang Ma Yajun Mao Yue Meng Xuyang Ning Ningchun Qi Zhicheng Qian Xiangxiang Ren Nasir Shaheed Changsong Shang Xiaofeng Shang Guofang Shen Lin Si Wenliang Sun Andi Tan Yi Tao Anqing Wang Meng Wang Qiuhong Wang Shaobo Wang Siguang Wang Wei Wang Xiuli Wang Zhou Wang Yuehuan Wei Weihao Wu Jingkai Xia Mengjiao Xiao Xiang Xiao Pengwei Xie Binbin Yan Xiyu Yan Jijun Yang Yong Yang Yukun Yao Zhengyun You Chunxu Yu Jumin Yuan Ying Yuan Zhe Yuan Xinning Zeng Dan Zhang Minzhen Zhang Peng Zhang Shibo Zhang Shu Zhang Tao Zhang Yang Zhang Yingxin Zhang Yuanyuan Zhang Li Zhao Qibin Zheng Jifang Zhou Ning Zhou Xiaopeng Zhou Yong Zhou Yubo Zhou Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai 200240 China School of Physics Sun Yat-Sen University Guangzhou 510275 China School of Physics and Astronomy Shanghai Jiao Tong University Key Laboratory for Particle Astrophysics and Cosmology (MoE) Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai 200240 China Shanghai Jiao Tong University Sichuan Research Institute Chengdu 610213 China Yalong River Hydropower Development Company Ltd. 288 Shuanglin Road Chengdu 610051 China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen University Zhuhai 519082 China School of Physics Nankai University Tianjin 300071 China Key Laboratory of Nuclear Physics and Ion-beam Application (MOE) Institute of Modern Physics Fudan University Shanghai 200433 China School of Physics Peking University Beijing 100871 China School of Physics Beihang University Beijing 102206 China International Research Center for Nuclei and Particles in the Cosmos and Beijing Key Laboratory of Advanced Nuclear Materials and Physics Beihang University Beijing 100191 China School of Physics and Microelectronics Zhengzhou University Zhengzhou Henan 450001 China School of Medical Instrument and Food Engineering University of Shanghai for Science and Technology Shanghai 200093 China Department of Physics University of Maryland College Park Maryland 20742 USA School of Mechanical Engineering Shanghai Jiao Tong University Shanghai 200240 China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of China Hefei 230026 China Department of Modern Physics University of Science and Technology of China Hefei 230026 China Research Center for Particle Science and Technology Institute of Frontier and Interdisciplinary Science Shandong University Qingdao 266237 Shandong China Key Laboratory of Particle Physics and Particle Irradiation of Ministry of Education Shandong University Qingdao 266237 Shandong China SJTU Pa

We report the search results of light dark matter through its interactions with shell electrons and nuclei, using the commissioning data from the PandaX-4T liquid xenon detector. Low energy events are selected to have an ionization-only signal between 60 to 200 photoelectrons, corresponding to a mean nuclear recoil energy from 0.77 to 2.54 keV and electronic recoil energy from 0.07 to 0.23 keV. With an effective exposure of 0.55 tonne·year, we set the most stringent limits within a mass range from 40 MeV/c2 to 10 GeV/c2 for pointlike dark matter-electron interaction, 100 MeV/c2 to 10 GeV/c2 for dark matter-electron interaction via a light mediator, and 3.2 to 4 GeV/c2 for dark matter-nucleon spin-independent interaction. For DM interaction with electrons, our limits are closing in on the parameter space predicted by the freeze-in and freeze-out mechanisms in the early Universe.

关键词： Dark matter particle dark matter Dark matter detectors

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Enhanced Ultra-High Energy Neutrino Search at the Askaryan Radio Array using Template-based Techniques 38

Enhanced Ultra-High Energy Neutrino Search at the Askaryan R...

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38th International Cosmic Ray Conference, ICRC 2023

作者： Kim, Myoungchul 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. Chiba University Chiba263-8522 Japan 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 Dept. of Physics Pennsylvania State University University ParkPA16802 United States Dept. of Astronomy and Astrophysics Pennsylvania State University University ParkPA16802 United States Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium 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 ManoaHI96822 United States

The Askaryan Radio Array (ARA) is a gigaton-size neutrino radio telescope situated near the geographic South Pole, which has been in operation since 2011. It is specifically designed to detect Askaryan emissions resulting from the interaction between ultra-high energy neutrinos (> 10 PeV) and Antarctic ice. Each of the five ARA stations is equipped with 16 antenna clusters arranged in a cubic configuration, approximately ∼200 m deep in the ice. In this analysis, we utilize data from two ARA stations with a total livetime of ∼10.5 years, representing a two times increase in exposure time compared to the previous ARA result. To enhance the detection of neutrinos at the ARA, we introduce the template method known as a matched filter, which was inspired by analysis methods used by the Laser Interferometer Gravitational-Wave Observatory (LIGO) Collaboration. This method entails the direct comparison of data with simulated neutrino signal templates, facilitating the identification of low signal-to-noise ratio (SNR) neutrino signatures, ultimately resulting in an improved low energy threshold. Our study presents the diffuse neutrino search results derived from the analysis of data, with an estimated factor of 4 sensitivity improvements above 10 PeV. These improvements were achieved through a factor of 2.3 improvement in analysis efficiency due to the application of the matched filter technique and a factor of 1.7 increase in livetime. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Signal to noise ratio

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Observation of Large-Scale Anisotropy of Proton above Tens of TeV with LHAASO-KM2A 38

Observation of Large-Scale Anisotropy of Proton above Tens o...

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38th International Cosmic Ray Conference, ICRC 2023

作者： He, Jiayin Zhao, Shiping Guo, Yingying Zhang, Yi Yuan, Qiang Cao, Zhen Aharonian, F. An, Q. Axikegu Bai, Y.X. Bao, Y.W. Bastieri, D. Bi, X.J. Bi, Y.J. Cai, J.T. Cao, Q. Cao, W.Y. Cao, Zhe Chang, J. Chang, J.F. Chen, A.M. Chen, E.S. Chen, Liang Chen, Lin Chen, Long Chen, M.J. Chen, M.L. Chen, Q.H. Chen, S.H. Chen, S.Z. Chen, T.L. Chen, Y. Cheng, N. Cheng, Y.D. Cui, M.Y. Cui, S.W. Cui, X.H. Cui, Y.D. Dai, B.Z. Dai, H.L. Dai, Z.G. Danzengluobu della Volpe, D. Dong, X.Q. Duan, K.K. Fan, J.H. Fan, Y.Z. Fang, J. Fang, K. Feng, C.F. Feng, L. Feng, S.H. Feng, X.T. Feng, Y.L. Gabici, S. Gao, B. Gao, C.D. Gao, L.Q. Gao, Q. Gao, W. Gao, W.K. Ge, M.M. Geng, L.S. Giacinti, G. Gong, G.H. Gou, Q.B. Gu, M.H. Guo, F.L. Guo, X.L. Guo, Y.Q. Guo, Y.Y. Han, Y.A. He, H.H. He, H.N. He, J.Y. He, X.B. He, Y. Heller, M. Hor, Y.K. Hou, B.W. Hou, C. Hou, X. Hu, H.B. Hu, Q. Hu, S.C. Huang, D.H. Huang, T.Q. Huang, W.J. Huang, X.T. Huang, X.Y. Huang, Y. Huang, Z.C. Ji, X.L. Jia, H.Y. Jia, K. Jiang, K. Jiang, X.W. Jiang, Z.J. Jin, M. Kang, M.M. Ke, T. Kuleshov, D. Kurinov, K. Li, B.B. Li, Cheng Li, Cong Li, D. Li, F. Li, H.B. Li, H.C. Li, H.Y. Li, J. Li, Jian Li, Jie Li, K. Li, W.L. Li, W.L. Li, X.R. Li, Xin Li, Y.Z. Li, Zhe Li, Zhuo Liang, E.W. Liang, Y.F. Lin, S.J. Liu, B. Liu, C. Liu, D. Liu, H. Liu, H.D. Liu, J. Liu, J.L. Liu, J.Y. Liu, M.Y. Liu, R.Y. Liu, S.M. Liu, W. Liu, Y. Liu, Y.N. Lu, R. Luo, Q. Lv, H.K. Ma, B.Q. Ma, L.L. Ma, X.H. Mao, J.R. Min, Z. Mitthumsiri, W. Mu, H.J. Nan, Y.C. Neronov, A. Ou, Z.W. Pang, B.Y. Pattarakijwanich, P. Pei, Z.Y. Qi, M.Y. Qi, Y.Q. Qiao, B.Q. Qin, J.J. Ruffolo, D. Sáiz, A. Semikoz, D. Shao, C.Y. Shao, L. Shchegolev, O. Sheng, X.D. Shu, F.W. Song, H.C. Stenkin, Yu.V. Stepanov, V. Su, Y. Sun, Q.N. Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences 9 Jiangsu Nanjing210023 China University of Science and Technology of China Anhui Hefei230026 China Institute of Frontier and Interdisciplinary Science Shandong University Shandong Qingdao266237 China Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China University of Chinese Academy of Sciences Beijing100049 China TIANFU Cosmic Ray Research Center Sichuan Chengdu China Dublin Institute for Advanced Studies 31 Fitzwilliam Place Dublin 2 Ireland Max-Planck-Institut for Nuclear Physics P.O. Box 103980 Heidelberg69029 Germany State Key Laboratory of Particle Detection and Electronics China School of Physical Science and Technology School of Information Science and Technology Southwest Jiaotong University Sichuan Chengdu610031 China School of Astronomy and Space Science Nanjing University Jiangsu Nanjing210023 China Center for Astrophysics Guangzhou University Guangdong Guangzhou510006 China Hebei Normal University Hebei Shijiazhuang050024 China Key Laboratory of Dark Matter and Space Astronomy Key Laboratory of Radio Astronomy Purple Mountain Observatory Chinese Academy of Sciences Jiangsu Nanjing210023 China Tsung-Dao Lee Institute School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Key Laboratory of Cosmic Rays [Tibet University Ministry of Education Tibet Lhasa850000 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Sun Yat-sen University 519000 Zhuhai Guangdong Guangzhou510275 China School of Physics and Astronomy Yunnan University Yunnan Kunming650091 China Département de Physique Nucléaire et Cor

We present a measurement for large-scale anisotropy of pure protons with the Large High Altitude Air Shower Observatory (LHAASO). We analyze the data collected from the full array of KM2A in one year’s operation. To select the proton data set, we employed a technique similar to the gamma/background discrimination method in KM2A, using a cut on the ratio of muonic and electron magnetic components. The purity of the proton sample is up to 90%, and the reconstructed energy is from 10 TeV to 270 TeV. We first perform the energy evolution analysis of the dipole anisotropy of protons at this energy range. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Anisotropy

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Benefits of Looking for Coincident Events, Taus, and Muons with the Askaryan Radio Array 38

Benefits of Looking for Coincident Events, Taus, and Muons w...

引用

38th International Cosmic Ray Conference, ICRC 2023

作者： Bishop, Abigail Cummings, Austin Krebs, Ryan Luszczak, William 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. Department of Physics Wisconsin IceCube Astrophysics Center University of Wisconsin-Madison MadisonWI53706 United States Departments of Physics and Astronomy & Astrophysics Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Department of Astronomy Ohio State University ColumbusOH43210 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 Dept. of Physics Pennsylvania State University University ParkPA16802 United States Dept. of Astronomy and Astrophysics Pennsylvania State University University ParkPA16802 United States Université Libre de Bruxelles Science Faculty CP230 BrusselsB-1050 Belgium 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 Tai

Ultra-High Energy (UHE) neutrinos over 1016 eV have yet to be observed but the Askaryan Radio Array (ARA) is one in-ice neutrino observatory attempting to make this discovery. In anticipation of a thorough full-observatory and full-livetime neutrino search, we estimate how many neutrino events can be detected accounting for secondary interactions, which are typically ignored in UHE neutrino simulations. Using the NuLeptonSim and PyREx simulation frameworks, we calculate the abundance and usefulness of cascades viewed by multiple ARA stations and observations made of taus, muons, and neutrinos generated during and after initial neutrino cascades. Analyses that include these scenarios benefit from a considerable increase in effective area at key ARA neutrino energies, one example being a 30% increase in ARA’s effective area when simulating taus and muons produced in 1019 eV neutrino interactions. These analysis techniques could be utilized by other in-ice radio neutrino observatories, as has been explored by NuRadioMC developers. Our contribution showcases full simulation results of neutrinos with energies 3 × 1017 - 1021 eV and visualizations of interesting triggered event topologies. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Neutrons

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