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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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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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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...

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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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Calculation of heavy meson light-cone distribution amplitudes from lattice QCD

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Physical Review D 2025年第3期111卷 034503-034503页

作者： Xue-Ying Han Jun Hua Xiangdong Ji Cai-Dian Lü Andreas Schäfer Yushan Su Wei Wang Ji Xu Yibo Yang Institute of High Energy Physics Chinese Academy of Sciences Beijing 100049 China School of Physical Sciences 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 University Regensburg D-93040 Regensburg Germany 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 Nuclear Science and Technology Lanzhou University Lanzhou 730000 China School of Physics and Microelectronics Zhengzhou University Zhengzhou Henan 450001 China CAS Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy of Sciences Beijing 100190 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 China

We develop an approach for calculating heavy quark effective theory (HQET) light-cone distribution amplitudes (LCDAs) by employing a sequential effective theory methodology. The theoretical foundation of the framework is established, elucidating how the quasidistribution amplitudes (quasi-DAs) with three scales can be utilized to compute HQET LCDAs. We provide theoretical support for this approach by demonstrating the rationale behind devising a hierarchical ordering for the three involved scales, discussing the factorization at each step, clarifying the underlying reason for obtaining HQET LCDAs in the final phase, and addressing potential theoretical challenges. The lattice QCD simulation aspect is explored in detail, and the computations of quasi-DAs are presented. We employ three fitting strategies to handle contributions from excited states and extract the bare matrix elements. For renormalization purposes, we apply hybrid renormalization schemes at short and long distance separations. To mitigate long-distance perturbations, we perform an extrapolation in λ=z·Pz and assess the stability against various parameters. After two-step matching, our results for HQET LCDAs are found in agreement with existing model parametrizations. The potential phenomenological implications of the results are discussed, shedding light on how these findings could impact our understanding of the strong interaction dynamics and physics beyond the standard model. It should be noted, however, that systematic uncertainties have not been accounted for yet.

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Development of Two-Dimensional Neutron Imager with a Sandwich Configuration

arXiv

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arXiv 2024年

作者： Kamiya, Y. Nishimura, R. Mitsui, S. Wang, Z. Morris, C.L. Makela, M. Clayton, S.M. Baldwin, J.K. Ito, T.M. Akamatsu, S. Iwase, H. Arai, Y. Murata, J. Asai, S. Department of Physics International Center for Elementary Particle Physics The University of Tokyo Bunkyo-ku Tokyo113-0033 Japan Ibaraki Tsukuba305-0801 Japan Hayama-tyô Kanagawa 240-0193 Japan Data Science and AI Innovation Research Promotion Center Shiga University Shiga Hikone522-8522 Japan Los Alamos National Laboratory Los AlamosNM87545 United States Department of Physics Rikkyo University Toshima-ku Tokyo171-8501 Japan

We have developed a two-dimensional neutron imager based on a semiconductor pixelated sensor, especially designed for experiments measuring of a spatial and a temporal behavior of quantum bound states of ultra-cold neutrons. Through these measurements, we expect to measure the ratio between the inertial and gravitational masses of neutrons and to test the equivalence principle in the quantum regime. As one of the principal neutron imagers, we fabricated a sensor with a sandwich configuration, named 10B-INTPIX4-sw, and tested its response to ultra-cold neutrons at the Los Alamos Neutron science center (LANSCE). We observed simultaneous events on both sandwiching sensors without significant loss of detection efficiency. The efficiency was evaluated to be about 16%, relative to the 10B/ZnS reference detector. The coincidence condition reduces its efficiency by a factor of about 3. © 2024, CC BY-NC-ND.

关键词： Neutrons

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Polarization Reconstruction of Askaryan Emission of Ultra-High Energy Neutrinos Using the Askaryan Radio Array 38

Polarization Reconstruction of Askaryan Emission of Ultra-Hi...

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38th International Cosmic Ray Conference, ICRC 2023

作者： Flaherty, Justin 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. 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. The Ohio State University 281 W Lane Ave 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 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 an ultra-high energy (> 10 PeV) neutrino detector located in the Dark Sector of the South Pole. It consists of five in-ice stations of antennas that are designed to detect radiation emitted by relativistic particle showers that are byproducts of neutrino interactions in the ice, which generate a cone of Cherenkov radiation in the radio regime (known as Askaryan radiation). The neutrino direction can be reconstructed through a combination of the direction of the Askaryan radiation, its polarization, and its frequency content. Since neutrinos are unaffected by electromagnetic forces and virtually unaffected by gravity, they travel in a straight line through the universe. This allows us to point them back towards potential sources. Through the use of radio pulser measurements, which are controlled radio emissions with a known polarization signature, we can evaluate our reconstruction techniques. Here I will show our reconstruction resolution after applying our reconstruction methods to pulser measurements. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Neutrons

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Exploring sub-GeV Dark Matter physics with Cosmic Ray and Future Telescopes

arXiv

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arXiv 2025年

作者： Wang, Guansen Su, Bing-Yu Zu, Lei Feng, Lei Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China National Centre for Nuclear Research ul. Pasteura 7 Warsaw02-093 Poland Joint Center for Particle Nuclear Physics and Cosmology Nanjing University Purple Mountain Observatory Nanjing210093 China

If sub-GeV Dark matter(DM) annihilates to the charged particles such as e+e−, µ+µ−, or π+π−, it generates an additional source of electrons and positrons in the cosmic ray (CR) population within our Milky Way. During propagation, these secondary electrons and positrons undergo reacceleration processes, boosting their energies to the GeV scale. Observatories like AMS-02 can detect these high-energy particles, enabling constraints on the properties of sub-GeV DM. By analyzing AMS-02 electron and positron data, the 95% upper limits on the DM annihilation cross-section have been established in the range of 10−28 to 10−27 cm3 s−1, corresponding to DM masses ranging from 100 MeV to 1 GeV. Meanwhile, MeV telescopes will provide complementary constraints on DM properties by detecting photon emissions from such annihilation processes. Notably, the sensitivity of future MeV gamma-ray observatories is projected to approach or match the constraints derived from CR data. © 2025, CC BY.

关键词： Cosmic rays

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New shape for cross-bispectra in Chern-Simons gravity

arXiv

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arXiv 2024年

作者： Christodoulidis, Perseas Gong, Jinn-Ouk Lin, Wei-Chen Mylova, Maria Sasaki, Misao Department of Science Education Ewha Womans University Seoul03760 Korea Republic of Korea Institute for Advanced Study Seoul02455 Korea Republic of Asia Pacific Center for Theoretical Physics Pohang37673 Korea Republic of Extreme Physics Institute Pusan National University Busan46241 Korea Republic of Department of Physics Pusan National University Busan46241 Korea Republic of The University of Tokyo Chiba Kashiwa277-8583 Japan Perimeter Institute for Theoretical Physics WaterlooONN2L 2Y5 Canada Center for Gravitational Physics and Quantum Information Yukawa Institute for Theoretical Physics Kyoto University Kyoto606-8502 Japan Leung Center for Cosmology Particle Astrophysics National Taiwan University Taipei10617 Taiwan

Chern-Simons gravity is known to suffer from graviton ghost production during inflation, which suppresses the parity-violating power spectrum at scales relevant to cosmic microwave background observations. In this work, we show that allowing the initial conditions of inflation to deviate from the standard Bunch-Davies state can enhance parity-violating non-Gaussianity in the scalar-tensor cross-bispectra. Our results reveal a significant additional contribution to the cross-bispectra in the flattened configuration, offering a new avenue to constrain parity-violating gravity. Copyright © 2024, The Authors. All rights reserved.

关键词： cosmology

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Effects of Biaxial Birefringence on Polarization Reconstruction for the Askaryan Radio Array 10

Effects of Biaxial Birefringence on Polarization Reconstruct...

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

作者： Salcedo-Gomez, Alan Flaherty, Justin Connolly, Amy 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. The Ohio State University 281 W Lane Ave 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

Ultra-high energy (UHE) neutrinos, with energies exceeding 1017 eV, offer unique insights into cosmic accelerators and the origins of ultra-high energy cosmic rays. The Askaryan Radio Array (ARA) is designed to detect UHE neutrinos by capturing radio signals generated by their interactions within Antarctic ice. Observations from the South Pole Ice Core Experiment (SPICE) pulsing campaign revealed unexpected polarization effects in detected radio pulses transmitted through polar ice. This paper explores the impact of biaxial birefringence in South Pole ice on the polarization of SPICE pulses. We present a model that accounts for biaxial birefringence effects, showing how signal polarization can rotate during propagation through the ice. We show that the biaxial birefringence model can potentially explain the unexpected polarization results observed in SPICE data and highlight the need to validate the model to enhance future analyses and detector designs. © Copyright owned by the author(s).

关键词： cosmology

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Observations of cosmic-ray Sun’s shadow with LHAASO-WCDA 38

Observations of cosmic-ray Sun’s shadow with LHAASO-WCDA

引用

38th International Cosmic Ray Conference, ICRC 2023

作者： Cui, Ming-Yang Xia, Jie He, Jia-Yin Shi, Guang-Lu Feng, Li Yuan, Qiang Zhang, Yi 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. Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China Key Laboratory of Particle Astrophyics & 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 University of Science and Technology of China Anhui Hefei230026 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 School of Physics and Astronomy Sun Yat-sen University Zhuhai519000 China School of Physics Guangdong Guangzhou510275 China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-sen Unive

During the propagation of cosmic rays (CRs) in the solar system, they are blocked by the Sun and deflected by the magnetic field, resulting in a shadow on the celestial map. As CRs travel from the vicinity of the Sun to the Earth, they encounter deflection from the coronal magnetic field (CMF), the interplanetary magnetic field (IMF), and finally the geomagnetic field (GMF). The extent of deflection is determined by the magnetic field’s intensity, direction, and energy of the CRs. Variations in the magnetic field cause corresponding changes in the position and size of the Sun’s shadow. By observing the Sun’s shadow of CRs, we can investigate the magnetic fields between the Sun and the Earth, complementing other measurements on these magnetic fields. Furthermore, it serves as a means to validate magnetic field models. The Large High Altitude Air Shower Observatory (LHAASO) is a new generation cosmic-ray and gamma-ray experiment in Daocheng, western China. With a vast Water Cherenkov Detector Array (WCDA) spanning 78,000 m2, LHAASO can successfully observe the significant Sun’s shadow within just a few days. Our study uses the WCDA to measure the Sun’s shadow effect caused by CRs over multiple Carrington rotation periods. Subsequently, we compare these results with simulations based on different magnetic field models. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Cosmic rays

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