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Astrophysics > Astrophysics of Galaxies

arXiv:2512.01638 (astro-ph)
[Submitted on 1 Dec 2025]

Title:Searching for EeV photons with Telescope Array Surface Detector and neural networks

Authors:Telescope Array Collaboration: R.U. Abbasi (1), T. Abu-Zayyad (1,2), M. Allen (2), J.W. Belz (2), D.R. Bergman (2), F. Bradfield (3), I. Buckland (2), W. Campbell (2), B.G. Cheon (4), K. Endo (3), A. Fedynitch (5,6), T. Fujii (3,7), K. Fujisue (5,6), K. Fujita (5), M. Fukushima (5), G. Furlich (2), A. Gálvez Ureña (8), Z. Gerber (2), N. Globus (9), T. Hanaoka (10), W. Hanlon (2), N. Hayashida (11), H. He (12), K. Hibino (11), R. Higuchi (12), D. Ikeda (11), D. Ivanov (2), S. Jeong (13), C.C.H. Jui (2), K. Kadota (14), F. Kakimoto (11), O. Kalashev (15), K. Kasahara (16), Y. Kawachi (3), K. Kawata (5), I. Kharuk (15), E. Kido (5), H.B. Kim (4), J.H. Kim (2), J.H. Kim (2), S.W. Kim (13), R. Kobo (3), I. Komae (3), K. Komatsu (17), K. Komori (10), A. Korochkin (18), C. Koyama (5), M. Kudenko (15), M. Kuroiwa (17), Y. Kusumori (10), M. Kuznetsov (15), Y.J. Kwon (19), K.H. Lee (4), M.J. Lee (13), B. Lubsandorzhiev (15), J.P. Lundquist (2,20), H. Matsushita (3), A. Matsuzawa (17), J.A. Matthews (2), J.N. Matthews (2), K. Mizuno (17), M. Mori (10), S. Nagataki (12), K. Nakagawa (3), M. Nakahara (3), H. Nakamura (10), T. Nakamura (21), T. Nakayama (17), Y. Nakayama (10), K. Nakazawa (10), T. Nonaka (5), S. Ogio (5), H. Ohoka (5), N. Okazaki (5), M. Onishi (5), A. Oshima (22), H. Oshima (5), S. Ozawa (23), I.H. Park (13), K.Y. Park (4), M. Potts (2), M. Przybylak (24), M.S. Pshirkov (15,25), J. Remington (2), C. Rott (2), G.I. Rubtsov (15), D. Ryu (26), H. Sagawa (5), N. Sakaki (5), R. Sakamoto (10), T. Sako (5), N. Sakurai (5), S. Sakurai (3), D. Sato (17), K. Sekino (5), T. Shibata (5), J. Shikita (3), H. Shimodaira (5), H.S. Shin
(3,7), K. Shinozaki (27), J.D. Smith (2), P. Sokolsky (2), B.T. Stokes (2), T.A. Stroman (2), H. Tachibana (3), K. Takahashi (5), M. Takeda (5), R. Takeishi (5), A. Taketa (28), M. Takita (5), Y. Tameda (10), K. Tanaka (29), M. Tanaka (30), M. Teramoto (10), S.B. Thomas (2), G.B. Thomson (2), P. Tinyakov (15,18), I. Tkachev (15), T. Tomida (17), S. Troitsky (15), Y. Tsunesada (3,7), S. Udo (11), F.R. Urban (8), M. Vrábel (27), D. Warren (12), K. Yamazaki (22), Y. Zhezher (5,15), Z. Zundel (2), J. Zvirzdin (2) ((1) Department of Physics, Loyola University-Chicago, Chicago, Illinois 60660, USA, (2) High Energy Astrophysics Institute and Department of Physics and Astronomy, University of Utah, Salt Lake City, Utah 84112-0830, USA, (3) Graduate School of Science, Osaka Metropolitan University, Sugimoto, Sumiyoshi, Osaka 558-8585, Japan, (4) Department of Physics and The Research Institute of Natural Science, Hanyang University, Seongdong-gu, Seoul 426-791, Korea, (5) Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan, (6) Institute of Physics, Academia Sinica, Taipei City 115201, Taiwan, (7) Nambu Yoichiro Institute of Theoretical and Experimental Physics, Osaka Metropolitan University, Sugimoto, Sumiyoshi, Osaka 558-8585, Japan, (8) CEICO, Institute of Physics, Czech Academy of Sciences, Prague 182 21, Czech Republic, (9) Institute of Astronomy, National Autonomous University of Mexico Ensenada Campus, Ensenada, BC 22860, Mexico, (10) Graduate School of Engineering, Osaka Electro-Communication University, Neyagawa-shi, Osaka 572-8530, Japan, (11) Faculty of Engineering, Kanagawa University, Yokohama, Kanagawa 221-8686, Japan, (12) Astrophysical Big Bang Laboratory, RIKEN, Wako, Saitama 351-0198, Japan, (13) Department of Physics, Sungkyunkwan University, Jang-an-gu, Suwon 16419, Korea, (14) Department of Physics, Tokyo City University, Setagaya-ku, Tokyo 158-8557, Japan, (15) Institute for Nuclear Research of the Russian Academy of Sciences, Moscow 117312, Russia, (16) Faculty of Systems Engineering and Science, Shibaura Institute of Technology, Minumaku, Tokyo 337-8570, Japan, (17) Academic Assembly School of Science and Technology Institute of Engineering, Shinshu University, Nagano, Nagano 380-8554, Japan, (18) Service de Physique Théorique, Université Libre de Bruxelles, Brussels 1050, Belgium, (19) Department of Physics, Yonsei University, Seodaemun-gu, Seoul 120-749, Korea, (20) Center for Astrophysics and Cosmology, University of Nova Gorica, Nova Gorica 5297, Slovenia, (21) Faculty of Science, Kochi University, Kochi, Kochi 780-8520, Japan, (22) College of Science and Engineering, Chubu University, Kasugai, Aichi 487-8501, Japan, (23) Quantum ICT Advanced Development Center, National Institute for Information and Communications Technology, Koganei, Tokyo 184-8795, Japan, (24) Doctoral School of Exact and Natural Sciences, University of Lodz, Lodz, Lodz 90-237, Poland, (25) Sternberg Astronomical Institute, Moscow M.V. Lomonosov State University, Moscow 119991, Russia, (26) Department of Physics, School of Natural Sciences, Ulsan National Institute of Science and Technology, UNIST-gil, Ulsan 689-798, Korea, (27) Astrophysics Division, National Centre for Nuclear Research, Warsaw 02-093, Poland, (28) Earthquake Research Institute, University of Tokyo, Bunkyo-ku, Tokyo 277-8582, Japan, (29) Graduate School of Information Sciences, Hiroshima City University, Hiroshima, Hiroshima 731-3194, Japan, (30) Institute of Particle and Nuclear Studies, KEK, Tsukuba, Ibaraki 305-0801, Japan)
et al. (30 additional authors not shown)  You must enable JavaScript to view entire author list.
View a PDF of the paper titled Searching for EeV photons with Telescope Array Surface Detector and neural networks, by Telescope Array Collaboration: R.U. Abbasi (1) and 283 other authors
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Abstract:Ultra-high-energy photons play an important role in probing astrophysical models and beyond-Standard-Model scenarios. We report updated limits on the diffuse photon flux using Telescope Array's Surface Detector data collected over 14 years of operation. Our method employs a neural network classifier to effectively distinguish between proton-induced and photon-induced events. The input data include both reconstructed composition-sensitive parameters and raw time-resolved signals registered by the Surface Detector stations. To mitigate biases from Monte Carlo simulations, we fine-tune the network with a subset of experimental data. The number of observed photon candidates is found to be consistent with the expected hadronic background, yielding upper limits on photon flux $\Phi_\gamma(E_\gamma > 10^{19} \text{eV}) < 2.3 \cdot 10^{-3} $, and $\Phi_\gamma(E_\gamma > 10^{20} \text{eV}) < 3.0 \cdot 10^{-4} $ $ (\text{km}^2 \cdot \text{sr} \cdot \text{yr})^{-1} $.
Subjects: Astrophysics of Galaxies (astro-ph.GA); High Energy Astrophysical Phenomena (astro-ph.HE); Instrumentation and Methods for Astrophysics (astro-ph.IM); High Energy Physics - Experiment (hep-ex)
Cite as: arXiv:2512.01638 [astro-ph.GA]
  (or arXiv:2512.01638v1 [astro-ph.GA] for this version)
  https://doi.org/10.48550/arXiv.2512.01638
arXiv-issued DOI via DataCite

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From: Ivan Kharuk [view email]
[v1] Mon, 1 Dec 2025 13:06:51 UTC (796 KB)
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