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Accurate and robust methods for direct background estimation in resonant anomaly detection

Physical Review D 2025年第9期111卷 094041-094041页

作者： Ranit Das Thorben Finke Marie Hein Gregor Kasieczka Michael Krämer Alexander Mück David Shih NHETC Department of Physics and Astronomy Rutgers University Piscataway New Jersey 08854 USA Institute for Theoretical Particle Physics and Cosmology RWTH Aachen University D-52056 Aachen Germany Institut für Experimentalphysik Universität Hamburg 22761 Hamburg Germany Center for Data and Computing in Natural Sciences (CDCS) 22607 Hamburg Germany

Resonant anomaly detection methods have great potential for enhancing the sensitivity of traditional bump hunt searches. A key component of these methods is a high quality background template used to produce an anomaly score. Using the LHC Olympics R&D dataset, we demonstrate that this background template can also be repurposed to directly estimate the background expectation in a simple cut and count setup. In contrast to a traditional bump hunt, no fit to the invariant mass distribution is needed, thereby avoiding the potential problem of background sculpting. Furthermore, direct background estimation allows working with large background rejection rates, where resonant anomaly detection methods typically show their greatest improvement in significance.

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Core to Cosmic Edge: SIMBA-C’s New Take on Abundance Profiles in the Intragroup Medium at z = 0

arXiv

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arXiv 2025年

作者： Padawer-Blatt, Aviv Shao, Zhiwei Hough, Renier T. Rennehan, Douglas Barré, Ruxin Saeedzadeh, Vida Babul, Arif Davé, Romeel Kobayashi, Chiaki Cui, Weiguang Mernier, François Gozaliasl, Ghassem Department of Physics and Astronomy University of Victoria VictoriaBCV8P 1A1 Canada Department of Astronomy School of Physics and Astronomy Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai Jiao Tong University Shanghai200240 China Center for Space Research North-West University Potchefstroom2520 South Africa Center for Computational Astrophysics Flatiron Institute New YorkNY10010 United States Department of Physics & Astronomy Johns Hopkins University BaltimoreMD21218 United States Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Department of Physics Indian Institute of Science Bangalore560012 India Department of Physics University of Helsinki P.O. Box 64 HelsinkiFI-00014 Finland Centre for Astrophysics Research Department of Physics Astronomy and Mathematics University of Hertfordshire HatfieldAL10 9AB United Kingdom Departamento de Física Téorica Universidad Autónoma de Madrid MadridE-28049 Spain Universidad Autónoma de Madrid Madrid28049 Spain NASA Goddard Space Flight Center GreenbeltMD20771 United States Department of Astronomy University of Marlyand College ParkMD20742 United States Department of Computer Science Aalto University P.O. Box 15400 EspooFI-00 076 Finland

We employ the SIMBA-C cosmological simulation to study the impact of its upgraded chemical enrichment model (Chem5) on the distribution of metals in the intragroup medium (IGrM). We investigate the projected X-ray emission-weighted abundance profiles of key elements over two decades in halo mass (1013 ≤ M500/M☉ ≤ 1015). Typically, SIMBA-C generates lower-amplitude abundance profiles than SIMBA with flatter cores, in better agreement with observations. For low-mass groups, both simulations over-enrich the IGrM with Si, S, Ca, and Fe compared to observations, a trend likely related to inadequate modeling of metal dispersal and mixing. We analyze the 3D mass-weighted abundance profiles, concluding that the lower SIMBA-C IGrM abundances are primarily a consequence of fewer metals in the IGrM, driven by reduced metal yields in Chem5, and the removal of the instantaneous recycling of metals approximation employed by SIMBA. Additionally, an increased IGrM mass in low-mass SIMBA-C groups is likely triggered by changes to the AGN and stellar feedback models. Our study suggests that a more realistic chemical enrichment model broadly improves agreement with observations, but physically motivated sub-grid models for other key processes, like AGN and stellar feedback and turbulent diffusion, are required to realistically reproduce observed group environments. © 2025, CC BY.

关键词： cosmology

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On thermodynamic self-consistency of generic axiomatic-nonextensive statistics

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Chinese physics C 2017年第5期41卷 73-90页

作者： Abdel Nasser Tawfik Hayam Yassin Eman R.Abo Elyazeed Egyptian Center for Theoretical Physics (ECTP) Modern University for Technology and Information (MTI) 11571 Cairo Egypt World Laboratory for Cosmology and Particle Physics (WLCAPP) 11571 Cairo Egypt Physics Department Faculty of Women for Arts Science and Education Ain Shams University 11577 Cairo Egypt

Generic axiomatic-nonextensive statistics introduces two asymptotic properties,to each of which a scaling function is *** first and second scaling properties are characterized by the exponents c and d,*** the thermodynamic limit,a grand-canonical ensemble can be *** thermodynamic properties of a relativistic ideal gas of hadron resonances are studied,*** is found that this generic statistics satisfies the requirements of the equilibrium *** aspects of the thermodynamic self-consistency are *** expressions are proposed for the statistical fits of various transverse momentum distributions measured in most-central collisions at different collision energies and colliding *** for the freezeout temperature（T_（ch）） and the baryon chemical potential（μ_b） and the exponents c and d are *** earlier are found compatible with the parameters deduced from Boltzmann-Gibbs（BG） statistics（extensive）,while the latter refer to generic *** resulting equivalence class（c,d） is associated with stretched exponentials,where Lambert function reaches its asymptotic *** some measurements,the resulting nonextensive entropy is linearly composed on extensive *** from power-scaling,the particle ratios and yields are excellent quantities to highlighting whether the particle production takes place（non）*** particle ratios and yields measured by the STAR experiment in central collisions at 200,62.4 and 7.7 GeV are fitted with this novel *** found that both c and d 〈 1,*** to neither BG-nor Tsallis-type statistics,but to（c,d）-entropy,where Lambert functions exponentially *** freezeout temperature and baryon chemical potential are found comparable with the ones deduced from BG statistics（extensive）.We conclude that the particle production at STAR energies is likely a nonextensive process but not necessarily BG or Tsallis

关键词： thermodynamic consistency asymptotic relativistic momentum quantities exponentially collision entropy generic

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DarkAI: Reconstructing the density, velocity and tidal field of dark matter from DESI-like bright galaxy sample

arXiv

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arXiv 2025年

作者： Shi, Feng Wang, Zitong Yang, Xiaohu Gu, Yizhou Wei, Chengliang Li, Ming Han, Jiaxin Wang, Huiyuan Zhang, Youcai Hong, Wensheng Wang, Yirong Li, Xiao-Dong School of Aerospace Science and Technology Xidian University Xi’an710126 China Shaanxi Key Laboratory of Space Extreme Detection Xidian University Xi’an710126 China Tsung-Dao Lee Institute School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai Jiao Tong University Shanghai200240 China Purple Mountain Observatory Nanjing210008 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Department of Astronomy Shanghai Jiao Tong University Shanghai200240 China Department of Astronomy University of Science and Technology of China Anhui Hefei230026 China Shanghai Astronomical Observatory Nandan Road 80 Shanghai200030 China School of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 China CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area SYSU Zhuhai519082 China

Reconstructing the dark matter density, velocity, and tidal (MTV) fields from galaxy surveys is essential for advancing our understanding of the large-scale structure of the Universe. In this work, we present a machine learning-based framework using a UNet convolutional neural network to reconstruct the MTV fields from mock samples of the DESI bright galaxy survey within the redshift range 0.1 −1. The velocity field reconstruction accurately captures large-scale coherent flows and small-scale turbulent features, exhibiting slopes of the grid-to-grid relationship close to unity and a scatter below ∼100 km s−1. Additionally, the tidal field is reconstructed without bias, successfully recovering the features of the large-scale cosmic web, including clusters, filaments, sheets, and voids. Our results confirm that the proposed framework effectively captures the large-scale distribution and dynamics of dark matter while addressing key systematic challenges. These advancements provide a reliable and robust tool for analyzing current and future galaxy surveys, paving the way for new insights into cosmic structure formation and evolution. Copyright © 2025, The Authors. All rights reserved.

关键词： Dark Matter

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Gravitational wave signatures from reheating in axion-Chern-Simons running-vacuum cosmology

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Physical Review D 2025年第4期111卷 043523-043523页

作者： Charalampos Tzerefos Theodoros Papanikolaou Spyros Basilakos Emmanuel N. Saridakis Nick E. Mavromatos Department of Physics National & Kapodistrian University of Athens Zografou Campus GR 157 73 Athens Greece National Observatory of Athens Lofos Nymfon 11852 Athens Greece Scuola Superiore Meridionale Largo S. Marcellino 10 80138 Napoli Italy Istituto Nazionale di Fisica Nucleare (INFN) Sezione di Napoli Via Cinthia 21 80126 Napoli Italy Academy of Athens Research Center for Astronomy and Applied Mathematics Soranou Efesiou 4 11527 Athens Greece School of Sciences European University Cyprus Diogenes Street Engomi 1516 Nicosia Cyprus CAS Key Laboratory for Researches in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei Anhui 230026 People’s Republic of China Departamento de Matemáticas Universidad Católica del Norte Avenida Angamos 0610 Casilla 1280 Antofagasta Chile Physics Division School of Applied Mathematical and Physical Sciences National Technical University of Athens Zografou Campus Athens 157 80 Greece Theoretical Particle Physics and Cosmology group Department of Physics King’s College London London WC2R 2LS United Kingdom

Within the context of a axion-Chern-Simons running-vacuum-model (RVM) cosmology, one expects an early matter dominated (eMD) reheating period after RVM inflation driven by the axion field. Treating thus in this work Chern-Simons RVM cosmology as an effective f(R) gravity theory characterized by logarithmic corrections of the spacetime curvature, we study the gravitational-wave (GW) signal induced by the nearly scale invariant inflationary adiabatic curvature perturbations during the transition from the eMD era driven by the axion to the late radiation-dominated era. Remarkably, by accounting for the extra GW scalaron polarization present within f(R) gravity theories, we find regions in the parameter space of the theory where one is met with a distinctive induced GW signal with a universal f6 high-frequency scaling compared to the f7 scaling present in general relativity (GR). In particular, for axion masses ma higher than 1 GeV and axion gauge couplings fa above 10−3 reduced Planck masses, one can produce induced GW spectra within the sensitivity bands of future GW observatories such as the Einstein Telescope (ET), the Laser Interferometer Space Antenna (LISA), the Big Bang Observer (BBO) and the Square Kilometer Arrays (SKA).

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Measurement of cosmic-ray energy spectrum with the TALE detector in hybrid mode 7

Measurement of cosmic-ray energy spectrum with the TALE dete...

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7th International Symposium on Ultra-High-Energy Cosmic Rays, UHECR 2024

作者： Oshima, H. Fujita, K. Ogio, S. Sako, T. Abbasi, R.U. Abe, Y. Abu-Zayyad, T. Allen, M. Arai, Y. Arimura, R. Barcikowski, E. Belz, J.W. Bergman, D.R. Blake, S.A. Buckland, I. Cheon, B.G. Chikawa, M. Fedynitch, A. Fujii, T. Fujisue, K. Fujita, K. Fujiwara, R. Fukushima, M. Furlich, G. Gerber, Z. Globus, N. Hanlon, W. Hayashida, N. He, H. Hibi, R. Hibino, K. Higuchi, R. Honda, K. Ikeda, D. Inoue, N. Ishii, T. Ito, H. Ivanov, D. Iwasaki, A. Jeong, H.M. Jeong, S. Jui, C.C.H. Kadota, K. Kakimoto, F. Kalashev, O. Kasahara, K. Kasami, S. Kawakami, S. Kawata, K. Kharuk, I. Kido, E. Kim, H.B. Kim, J.H. Kim, S.W. Kimura, Y. Komae, I. Komori, K. Kusumori, Y. Kuznetsov, M. Kwon, Y.J. Lee, K.H. Lee, M.J. Lubsandorzhiev, B. Lundquist, J.P. Matsuyama, T. Matthews, J.A. Matthews, J.N. Mayta, R. Miyashita, K. Mizuno, K. Mori, M. Murakami, M. Myers, I. Nagataki, S. Nakai, K. Nakamura, T. Nishio, E. Nonaka, T. Ogio, S. Ohoka, H. Okazaki, N. Oku, Y. Okuda, T. Omura, Y. Onishi, M. Ono, M. Oshima, A. Oshima, H. Ozawa, S. Park, I.H. Park, K.Y. Pshirkov, M.S. Remington, J. Rodriguez, D.C. Rott, C. Rubtsov, G.I. Ryu, D. Sagawa, H. Saito, R. Sakaki, N. Sako, T. Sakurai, N. Sato, D. Sato, K. Sato, S. Sekino, K. Shah, P.D. Shibata, N. Shibata, T. Shikita, J. Shimodaira, H. Shin, B.K. Shin, H.S. Shinto, D. Smith, J.D. Sokolsky, P. Stokes, B.T. Stroman, T.A. Takagi, Y. Takahashi, K. Takamura, M. Takeda, M. Takeishi, R. Taketa, A. Takita, M. Tameda, Y. Tanaka, K. Tanaka, M. Thomas, S.B. Thomson, G.B. Tinyakov, P. Tkachev, I. Tokuno, H. Tomida, T. Troitsky, S. Tsuda, R. Tsunesada, Y. Udo, S. Urban, F. Vaiman, I.A. Warren, D. Wong, T. Yamazaki, K. Yashiro, K. Yoshida, F. Zhezher, Y. Zundel, Z. Institute for Cosmic Ray Research University of Tokyo 5-1-5 Kashiwa-no-ha Chiba Kashiwa Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States Academic Assembly School of Science and Technology Institute of Engineering Shinshu University Nagano Nagano380-8554 Japan High Energy Astrophysics Institute Department of Physics and Astronomy University of Utah Salt Lake CityUT84112-0830 United States Graduate School of Science Osaka Metropolitan University Sugimoto Sumiyoshi Osaka558-8585 Japan Department of Physics The Research Institute of Natural Science Hanyang University Seongdong-gu Seoul426-791 Korea Republic of Institute for Cosmic Ray Research University of Tokyo Chiba Kashiwa277-8582 Japan Institute of Physics Academia Sinica Taipei City115201 Taiwan Nambu Yoichiro Institute of Theoretical and Experimental Physics Osaka Metropolitan University Sugimoto Sumiyoshi Osaka558-8585 Japan Astrophysical Big Bang Laboratory RIKEN Saitama Wako351-0198 Japan Faculty of Engineering Kanagawa University Kanagawa Yokohama221-8686 Japan Interdisciplinary Graduate School of Medicine and Engineering University of Yamanashi Yamanashi Kofu400-8511 Japan The Graduate School of Science and Engineering Saitama University Saitama Saitama338-8570 Japan Department of Physics SungKyunKwan University Jang-an-gu Suwon16419 Korea Republic of Department of Physics Tokyo City University Setagaya-ku Tokyo158-8557 Japan Institute for Nuclear Research Russian Academy of Sciences Moscow117312 Russia Faculty of Systems Engineering and Science Shibaura Institute of Technology Minato-ku Tokyo337-8570 Japan Graduate School of Engineering Osaka Electro-Communication University Osaka Neyagawa-shi572-8530 Japan Service de Physique Théorique Université Libre de Bruxelles Brussels Belgium Department of Physics Yonsei University Seodaemun-gu Seoul120-749 Korea Republic of Center for Astrophysics and Cosmology University of N

The TA Low-energy Extension (TALE) experiment extends the reach of the TA experiment on the low-energy side to below 1016 eV. A primary objective of TALE is to study the transition from galactic to extragalactic cosmic rays. The TALE detector is a hybrid observatory composed of fluorescence telescopes and a surface detector array of scintillation counters. The surface detectors are arranged with inter-counter spacing optimized for hybrid energy spectrum measurements in the low-energy region. We analyzed data collected between November 2018 and May 2023, corresponding to 1,247 hours of operation. In this presentation, we will show the results of the cosmic ray energy spectrum measurement using the TALE hybrid detector. This measurement will play an important role in understanding the transition from cosmic rays of galactic origin to those of extragalactic origin. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). All rights for text and data mining, AI training, and similar technologies for commercial purposes, are reserved.

关键词： Cosmic ray measurement

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Study of the semileptonic decay D0→K¯0π−e+νe

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Journal of High Energy physics 2025年第3期2025卷 1-20页

作者： Ablikim, M. Achasov, M.N. Adlarson, P. Afedulidis, O. Ai, X.C. Aliberti, R. Amoroso, A. Bai, Y. Bakina, O. Balossino, I. Ban, Y. Bao, H.-R. Batozskaya, V. Begzsuren, K. Berger, N. Berlowski, M. Bertani, M. Bettoni, D. Bianchi, F. Bianco, E. Bortone, A. Boyko, I. Briere, R.A. Brueggemann, A. Cai, H. Cai, X. Calcaterra, A. Cao, G.F. Cao, N. Cetin, S.A. Chai, X.Y. Chang, J.F. Che, G.R. Che, Y.Z. Chelkov, G. Chen, Chao Chen, C.H. Chen, G. Chen, H.S. Chen, H.Y. Chen, M.L. Chen, S.J. Chen, S.L. Chen, S.M. Chen, T. Chen, X.R. Chen, X.T. Chen, Y.B. Chen, Y.Q. Chen, Z.J. Choi, S.K. Cibinetto, G. Cossio, F. Cui, J.J. Dai, H.L. Dai, J.P. Dbeyssi, A. de Boer, R.E. Dedovich, D. Deng, C.Q. Deng, Z.Y. Denig, A. Denysenko, I. Destefanis, M. De Mori, F. Ding, B. Ding, X.X. Ding, Y. Dong, J. Dong, L.Y. Dong, M.Y. Dong, X. Du, M.C. Du, S.X. Duan, Y.Y. Duan, Z.H. Egorov, P. Fan, G.F. Fan, J.J. Fan, Y.H. Fang, J. Fang, S.S. Fang, W.X. Fang, Y. Fang, Y.Q. Farinelli, R. Fava, L. Feldbauer, F. Felici, G. Feng, C.Q. Feng, J.H. Feng, Y.T. Fritsch, M. Fu, C.D. Fu, J.L. Fu, Y.W. Gao, H. Gao, X.B. Gao, Y.N. Gao, Yang Garbolino, S. Garzia, I. Ge, P.T. Ge, Z.W. Geng, C. Gersabeck, E.M. Gilman, A. Goetzen, K. Gong, L. Gong, W.X. Gradl, W. Gramigna, S. Greco, M. Gu, M.H. Gu, Y.T. Guan, C.Y. Guo, A.Q. Guo, L.B. Guo, M.J. Guo, R.P. Guo, Y.P. Guskov, A. Gutierrez, J. Han, K.L. Han, T.T. Hanisch, F. Hao, X.Q. Harris, F.A. He, K.K. He, K.L. Heinsius, F.H. Heinz, C.H. Heng, Y.K. Herold, C. Holtmann, T. Hong, P.C. Hou, G.Y. Hou, X.T. Hou, Y.R. Hou, Z.L. Hu, B.Y. Hu, H.M. Hu, J.F. Hu, Q.P. Hu, S.L. Hu, T. Hu, Y. Huang, G.S. Huang, K.X. Huang, L.Q. Huang, P. Huang, X.T. Huang, Y.P. Huang, Y.S. Hussain, T. Hölzken, F. Hüsken, N. in der Wiesche, N. Jackson, J. Janchiv, S. Ji, Q. Ji, Q.P. Ji, W. Ji, X.B. Ji, X.L. Ji, Y.Y. Jia, X.Q. Jia, Z.K. Jiang, D. Jiang, H.B. Jiang, P.C. Jiang, S.S. Jiang, T.J. Jiang, X.S. Jiang, Y. Jiao, J.B. Jiao, J.K. Jiao, Z. Jin, S. Jin, Y. Jing, M.Q. Jing, X.M. Johansson, T. Kabana, S. Kalantar-Nayestanaki, N. Kang, X.L. Kang, X.S Institute of High Energy Physics Beijing 100049 China Beihang University Beijing 100191 China Bochum Ruhr-University Bochum D-44780 Germany Budker Institute of Nuclear Physics SB RAS (BINP) Novosibirsk 630090 Russian Federation Carnegie Mellon University Pittsburgh 15213 PA United States Central China Normal University Wuhan 430079 China Central South University Changsha 410083 China China Center of Advanced Science and Technology Beijing 100190 China China University of Geosciences Wuhan 430074 China Chung-Ang University Seoul 06974 South Korea COMSATS University Islamabad Lahore Campus Defence Road Off Raiwind Road Lahore 54000 Pakistan Fudan University Shanghai 200433 China GSI Helmholtzcentre for Heavy Ion Research GmbH Darmstadt D-64291 Germany Guangxi Normal University Guilin 541004 China Guangxi University Nanning 530004 China Hangzhou Normal University Hangzhou 310036 China Hebei University Baoding 071002 China Helmholtz Institute Mainz Staudinger Weg 18 Mainz D-55099 Germany Henan Normal University Xinxiang 453007 China Henan University Kaifeng 475004 China Henan University of Science and Technology Luoyang 471003 China Henan University of Technology Zhengzhou 450001 China Huangshan College Huangshan 245000 China Hunan Normal University Changsha 410081 China Hunan University Changsha 410082 China Indian Institute of Technology Madras Chennai 600036 India Indiana University Bloomington 47405 IN United States INFN Laboratori Nazionali di Frascati Frascati I-00044 Italy INFN Sezione di Perugia Perugia I-06100 Italy University of Perugia Perugia I-06100 Italy INFN Sezione di Ferrara Ferrara I-44122 Italy University of Ferrara Ferrara I-44122 Italy Inner Mongolia University Hohhot 010021 China Institute of Modern Physics Lanzhou 730000 China Institute of Physics and Technology Peace Avenue 54B Ulaanbaatar 13330 Mongolia Instituto de Alta Investigación Universidad de Tarapacá Casilla 7D Arica 100

We report an improved study of the semileptonic decay D0→K¯0π−e+νe based on a sample of 7.9 fb−1 of e+e− annihilation data collected at a center-of-mass energy of 3.773 GeV with the BESIII detector at the BEPC... 详细信息

We report an improved study of the semileptonic decay D0→K¯0π−e+νe based on a sample of 7.9 fb⁻¹ of e⁺e⁻ annihilation data collected at a center-of-mass energy of 3.773 GeV with the BESIII detector at the BEPCII collider. The branching fraction of this decay is measured to be BD0→K¯0π−e+νe = (1.444 ± 0.022_stat ± 0.024_syst)%, which is the most precise to date, where the first uncertainty is statistical and the second is systematic. Based on investigation of the decay dynamics, we find that the decay is dominated by the K^*(892)⁻ component and present an improved measurement of its branching fraction to be BD0→K∗892−e+νe = (2.039 ± 0.032_stat± 0.034_syst)%. We also determine the ratios of the hadronic form factors for the K^*(892)⁻e⁺ν_e decay to be r_V = V(0)/A₁(0) = 1.48 ± 0.05_stat± 0.02_syst and r₂ = A₂(0)/A₁(0) = 0.70 ± 0.04_stat± 0.02_syst, where V(0) is the vector form factor and A_1,2(0) are the axial form factors. In addition, the K¯0π−S-wave component is found to account for (5.87 ± 0.32_stat± 0.16_syst)% of the total decay rate, corresponding to a branching fraction of BD0→K¯0π−S−wavee+νe = (0.085 ± 0.005_stat± 0.003_syst)%. © The Author(s) 2025.

关键词： Charm physics e+-e− Experiments

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Measurement of cosmic rays with energies down to the PeV region using the TALE-infill SD array 7

Measurement of cosmic rays with energies down to the PeV reg...

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7th International Symposium on Ultra-High-Energy Cosmic Rays, UHECR 2024

作者： Kawachi, Yusuke Abbasi, R.U. Abu-Zayyad, T. Allen, M. Belz, J.W. Bergman, D.R. Buckland, I. Campbell, W. Cheon, B.G. Endo, K. Fedynitch, A. Fujii, T. Fujisue, K. Fujita, K. Fukushima, M. Furlich, G. Gerber, Z. Globus, N. Hanlon, W. Hayashida, N. He, H. Hibino, K. Higuchi, R. Ikeda, D. Ishii, T. Ivanov, D. Jeong, S. Jui, C.C.H. Kadota, K. Kakimoto, F. Kalashev, O. Kasahara, K. Kawachi, Y. Kawata, K. Kharuk, I. Kido, E. Kim, H.B. Kim, J.H. Kim, S.W. Kobo, R. Komae, I. Komatsu, K. Komori, K. Koyama, C. Kudenko, M. Kuroiwa, M. Kusumori, Y. Kuznetsov, M. Kwon, Y.J. Lee, K.H. Lee, M.J. Lubsandorzhiev, B. Lundquist, J.P. Matsuzawa, A. Matthews, J.A. Matthews, J.N. Mizuno, K. Mori, M. Murakami, M. Nagataki, S. Nakahara, M. Nakamura, T. Nakayama, T. Nakayama, Y. Nonaka, T. Ogio, S. Ohoka, H. Okazaki, N. Onishi, M. Oshima, A. Oshima, H. Ozawa, S. Park, I.H. Park, K.Y. Potts, M. Przybylak, M. Pshirkov, M.S. Remington, J. Rott, C. Rubtsov, G.I. Ryu, D. Sagawa, H. Sakaki, N. Sakamoto, R. Sako, T. Sakurai, N. Sakurai, S. Sato, D. Sato, S. Sekino, K. Shibata, T. Shikita, J. Shimodaira, H. Shin, B.K. Shin, H.S. Shinozaki, K. Smith, J.D. Sokolsky, P. Stokes, B.T. Stroman, T.A. Takagi, Y. Takahashi, K. Takeda, M. Takeishi, R. Taketa, A. Takita, M. Tameda, Y. Tanaka, K. Tanaka, M. Thomas, S.B. Thomson, G.B. Tinyakov, P. Tkachev, I. Tomida, T. Troitsky, S. Tsunesada, Y. Udo, S. Urban, F. Vaiman, I.A. Vrabel, M. Warren, D. Yamazaki, K. Zhezher, Y. Zundel, Z. Zvirzdin, J. Graduate School of Science Osaka Metropolitan University 3-3-138 Sugimoto Sumiyoshi-ku Osaka558-8585 Japan Department of Physics Loyola University Chicago ChicagoIL60660 United States High Energy Astrophysics Institute Department of Physics and Astronomy University of Utah Salt Lake CityUT84112-0830 United States Department of Physics The Research Institute of Natural Science Hanyang University Seongdong-gu Seoul426-791 Korea Republic of Graduate School of Science Osaka Metropolitan University Sugimoto Sumiyoshi Osaka558-8585 Japan Institute for Cosmic Ray Research University of Tokyo Chiba Kashiwa277-8582 Japan Institute of Physics Academia Sinica Taipei City115201 Taiwan Nambu Yoichiro Institute of Theoretical and Experimental Physics Osaka Metropolitan University Sugimoto Sumiyoshi Osaka558-8585 Japan Astrophysical Big Bang Laboratory RIKEN Saitama Wako351-0198 Japan Faculty of Engineering Kanagawa University Kanagawa Yokohama221-8686 Japan Interdisciplinary Graduate School of Medicine and Engineering University of Yamanashi Yamanashi Kofu400-8511 Japan Department of Physics Sungkyunkwan University Jang-an-gu Suwon16419 Korea Republic of Department of Physics Tokyo City University Setagaya-ku Tokyo158-8557 Japan Institute for Nuclear Research Russian Academy of Sciences Moscow117312 Russia Faculty of Systems Engineering and Science Shibaura Institute of Technology Minato-ku Tokyo337-8570 Japan Academic Assembly School of Science and Technology Institute of Engineering Shinshu University Nagano Nagano380-8554 Japan Graduate School of Engineering Osaka Electro-Communication University Osaka Neyagawa-shi572-8530 Japan Service de Physique Theorique Universite Libre de Bruxelles Brussels1050 Belgium Department of Physics Yonsei University Seodaemun-gu Seoul120-749 Korea Republic of Center for Astrophysics and Cosmology University of Nova Gorica Nova Gorica5297 Slovenia Faculty of Science Kochi University Koch

The Telescope Array Low-energy Extension (TALE) experiment is a project that extends the Telescope Array (TA) experiment to observe cosmic rays with energies down to 1016.5 eV using 10 fluorescence detectors (FDs) and 80 surface detectors (SDs). The TALE-infill SD array, consisting of 50 SDs arranged in a grid pattern with 100-meter spacing, has been installed to extend observations to lower energies, covering the PeV energy region. The extension as TALE-infill enables precise measurements of the energy spectrum, mass composition, and arrival direction anisotropy of cosmic rays around the knee, with the aim of investigating the origin of cosmic rays and the physical mechanisms responsible for the knee feature. In this paper, we report on the observational status of the TALE-infill array, using the first data from November 2023 to Jun 2024. © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). All rights for text and data mining, AI training, and similar technologies for commercial purposes, are reserved.

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Measurement of the branching fraction of D⁺→ τ⁺ν_τ

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Journal of High Energy physics 2025年第1期2025卷 1-16页

作者： Ablikim, M. Achasov, M.N. Adlarson, P. Afedulidis, O. Ai, X.C. Aliberti, R. Amoroso, A. Bai, Y. Bakina, O. Balossino, I. Ban, Y. Bao, H.-R. Batozskaya, V. Begzsuren, K. Berger, N. Berlowski, M. Bertani, M. Bettoni, D. Bianchi, F. Bianco, E. Bortone, A. Boyko, I. Briere, R.A. Brueggemann, A. Cai, H. Cai, X. Calcaterra, A. Cao, G.F. Cao, N. Cetin, S.A. Chai, X.Y. Chang, J.F. Che, G.R. Che, Y.Z. Chelkov, G. Chen, Chao Chen, C.H. Chen, G. Chen, H.S. Chen, H.Y. Chen, M.L. Chen, S.J. Chen, S.L. Chen, S.M. Chen, T. Chen, X.R. Chen, X.T. Chen, Y.B. Chen, Y.Q. Chen, Z.J. Chen, Z.Y. Choi, S.K. Cibinetto, G. Cossio, F. Cui, J.J. Dai, H.L. Dai, J.P. Dbeyssi, A. de Boer, R.E. Dedovich, D. Deng, C.Q. Deng, Z.Y. Denig, A. Denysenko, I. Destefanis, M. De Mori, F. Ding, B. Ding, X.X. Ding, Y. Dong, J. Dong, L.Y. Dong, M.Y. Dong, X. Du, M.C. Du, S.X. Duan, Y.Y. Duan, Z.H. Egorov, P. Fan, Y.H. Fang, J. Fang, S.S. Fang, W.X. Fang, Y. Farinelli, R. Fava, L. Feldbauer, F. Felici, G. Feng, C.Q. Feng, J.H. Feng, Y.T. Fritsch, M. Fu, C.D. Fu, J.L. Fu, Y.W. Gao, H. Gao, X.B. Gao, Y.N. Gao, Yang Garbolino, S. Garzia, I. Ge, L. Ge, P.T. Ge, Z.W. Geng, C. Gersabeck, E.M. Gilman, A. Goetzen, K. Gong, L. Gong, W.X. Gradl, W. Gramigna, S. Greco, M. Gu, M.H. Gu, Y.T. Guan, C.Y. Guo, A.Q. Guo, L.B. Guo, M.J. Guo, R.P. Guo, Y.P. Guskov, A. Gutierrez, J. Han, K.L. Han, T.T. Hanisch, F. Hao, X.Q. Harris, F.A. He, K.K. He, K.L. Heinsius, F.H. Heinz, C.H. Heng, Y.K. Herold, C. Holtmann, T. Hong, P.C. Hou, G.Y. Hou, X.T. Hou, Y.R. Hou, Z.L. Hu, B.Y. Hu, H.M. Hu, J.F. Hu, Q.P. Hu, S.L. Hu, T. Hu, Y. Huang, G.S. Huang, K.X. Huang, L.Q. Huang, X.T. Huang, Y.P. Huang, Y.S. Hussain, T. Hölzken, F. Hüsken, N. in der Wiesche, N. Jackson, J. Janchiv, S. Jeong, J.H. Ji, Q. Ji, Q.P. Ji, W. Ji, X.B. Ji, X.L. Ji, Y.Y. Jia, X.Q. Jia, Z.K. Jiang, D. Jiang, H.B. Jiang, P.C. Jiang, S.S. Jiang, T.J. Jiang, X.S. Jiang, Y. Jiao, J.B. Jiao, J.K. Jiao, Z. Jin, S. Jin, Y. Jing, M.Q. Jing, X.M. Johansson, T. Kabana, S. Kalantar-Nayestanaki, N. Kang, X.L. Kang, X.S. Kavatsyuk Institute of High Energy Physics Beijing 100049 China Beihang University Beijing 100191 China Bochum Ruhr-University Bochum D-44780 Germany Budker Institute of Nuclear Physics SB RAS (BINP) Novosibirsk 630090 Russian Federation Carnegie Mellon University Pittsburgh 15213 PA United States Central China Normal University Wuhan 430079 China Central South University Changsha 410083 China China Center of Advanced Science and Technology Beijing 100190 China China University of Geosciences Wuhan 430074 China Chung-Ang University Seoul 06974 South Korea COMSATS University Islamabad Lahore Campus Defence Road Off Raiwind Road Lahore 54000 Pakistan Fudan University Shanghai 200433 China GSI Helmholtzcentre for Heavy Ion Research GmbH Darmstadt D-64291 Germany Guangxi Normal University Guilin 541004 China Guangxi University Nanning 530004 China Hangzhou Normal University Hangzhou 310036 China Hebei University Baoding 071002 China Helmholtz Institute Mainz Staudinger Weg 18 Mainz D-55099 Germany Henan Normal University Xinxiang 453007 China Henan University Kaifeng 475004 China Henan University of Science and Technology Luoyang 471003 China Henan University of Technology Zhengzhou 450001 China Huangshan College Huangshan 245000 China Hunan Normal University Changsha 410081 China Hunan University Changsha 410082 China Indian Institute of Technology Madras Chennai 600036 India Indiana University Bloomington 47405 IN United States INFN Laboratori Nazionali di Frascati Frascati I-00044 Italy INFN Sezione di Perugia Perugia I-06100 Italy University of Perugia Perugia I-06100 Italy INFN Sezione di Ferrara Ferrara I-44122 Italy University of Ferrara Ferrara I-44122 Italy Inner Mongolia University Hohhot 010021 China Institute of Modern Physics Lanzhou 730000 China Institute of Physics and Technology Peace Avenue 54B Ulaanbaatar 13330 Mongolia Instituto de Alta Investigación Universidad de Tarapacá Casilla 7D Arica 100

By analyzing e+e− collision data with an integrated luminosity of 7.9 fb−1 collected with the BESIII detector at the center-of-mass energy of 3.773 GeV, the branching fraction of D+→ τ+ντ is determined as B = (9.9... 详细信息

By analyzing e⁺e⁻ collision data with an integrated luminosity of 7.9 fb⁻¹ collected with the BESIII detector at the center-of-mass energy of 3.773 GeV, the branching fraction of D⁺→ τ⁺ν_τ is determined as B = (9.9 ± 1.1_stat± 0.5_syst) × 10⁻⁴. Using the most precise result B(D⁺→ μ⁺ν_μ) = (3.981 ± 0.079_stat± 0.040_syst) × 10⁻⁴ [1], we determine R_τ/μ = Γ(D⁺ → τ⁺ν_τ)/Γ(D⁺ → μ⁺ν_μ) = 2.49 ± 0.31, achieving a factor of two improvement in precision compared to the previous BESIII result. This measurement is in agreement with the standard model prediction of lepton flavor universality within one standard deviation. © The Author(s) 2025.

关键词： Branching fraction Charm physics e+-e− Experiments Flavour physics

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The Quantum Trellis: A classical algorithm for sampling the parton shower with interference effects

arXiv

引用

arXiv 2021年

作者： Macaluso, Sebastian Cranmer, Kyle Center for Cosmology and Particle Physics & Center for Data Science New York University United States

Simulations of high-energy particle collisions, such as those used at the Large Hadron Collider, are based on quantum field theory;however, many approximations are made in practice. For example, the simulation of the parton shower, which gives rise to objects called 'jets', is based on a semi-classical approximation that neglects various interference effects. While there is a desire to incorporate interference effects, new computational techniques are needed to cope with the exponential growth in complexity associated to quantum processes. We present a classical algorithm called the quantum trellis to efficiently compute the un-normalized probability density over N-body phase space including all interference effects, and we pair this with an MCMC-based sampling strategy. This provides a potential path forward for classical computers and a strong baseline for approaches based on quantum computing. Copyright © 2021, The Authors. All rights reserved.

关键词： Phase space methods

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