Measurements of the charge ratio and polarization of cosmic-ray muons with the Super-Kamiokande detector

We present the results of the charge ratio (<a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mi>R</a:mi></a:math>) and polarization (<c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:msubsup><c:mi>P</c:mi><c:mn>0</c:mn><c:mi>μ</c:mi></c:msubsup></c:math>) measurements using decay electron events collected between September 2008 and June 2022 with the Super-Kamiokande detector. Because of its underground location and long operation, we are able to perform high-precision measurements by accumulating cosmic-ray muons. We measured the muon charge ratio to be <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"><e:mi>R</e:mi><e:mo>=</e:mo><e:mn>1.32</e:mn><e:mo>±</e:mo><e:mn>0.02</e:mn><e:mo stretchy="false">(</e:mo><e:mrow><e:mi>stat</e:mi></e:mrow><e:mo>+</e:mo><e:mrow><e:mi>syst</e:mi></e:mrow><e:mo stretchy="false">)</e:mo></e:math> at <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"><i:msub><i:mi>E</i:mi><i:mi>μ</i:mi></i:msub><i:mi>cos</i:mi><i:msub><i:mi>θ</i:mi><i:mtext>Zenith</i:mtext></i:msub><i:mo>=</i:mo><i:msubsup><i:mn>0.7</i:mn><i:mrow><i:mo>−</i:mo><i:mn>0.2</i:mn></i:mrow><i:mrow><i:mo>+</i:mo><i:mn>0.3</i:mn></i:mrow></i:msubsup><i:mtext> </i:mtext><i:mtext> </i:mtext><i:mi>TeV</i:mi></i:math>, where <k:math xmlns:k="http://www.w3.org/1998/Math/MathML" display="inline"><k:msub><k:mi>E</k:mi><k:mi>μ</k:mi></k:msub></k:math> is the muon energy and <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:msub><m:mi>θ</m:mi><m:mtext>Zenith</m:mtext></m:msub></m:math> is the zenith angle of incoming cosmic-ray muons. This result is consistent with the Honda flux model while indicating a tension with the <o:math xmlns:o="http://www.w3.org/1998/Math/MathML" display="inline"><o:mi>π</o:mi><o:mi>K</o:mi></o:math> model of <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"><q:mn>1.9</q:mn><q:mi>σ</q:mi></q:math>. We also measured the muon polarization at the production location to be <s:math xmlns:s="http://www.w3.org/1998/Math/MathML" display="inline"><s:mrow><s:msubsup><s:mrow><s:mi>P</s:mi></s:mrow><s:mrow><s:mn>0</s:mn></s:mrow><s:mrow><s:mi>μ</s:mi></s:mrow></s:msubsup><s:mo>=</s:mo><s:mn>0.52</s:mn><s:mo>±</s:mo><s:mn>0.02</s:mn><s:mtext> </s:mtext><s:mtext> </s:mtext><s:mo stretchy="false">(</s:mo><s:mrow><s:mi>stat</s:mi></s:mrow><s:mo>+</s:mo><s:mrow><s:mi>syst</s:mi></s:mrow><s:mo stretchy="false">)</s:mo></s:mrow></s:math> at the muon momentum of <w:math xmlns:w="http://www.w3.org/1998/Math/MathML" display="inline"><w:msubsup><w:mn>0.9</w:mn><w:mrow><w:mo>−</w:mo><w:mn>0.1</w:mn></w:mrow><w:mrow><w:mo>+</w:mo><w:mn>0.6</w:mn></w:mrow></w:msubsup><w:mtext> </w:mtext><w:mtext> </w:mtext><w:mi>TeV</w:mi><w:mo>/</w:mo><w:mi>c</w:mi></w:math> at the surface of the mountain; this also suggests a tension with the Honda flux model of <y:math xmlns:y="http://www.w3.org/1998/Math/MathML" display="inline"><y:mn>1.5</y:mn><y:mi>σ</y:mi></y:math>. This is the most precise measurement ever to experimentally determine the cosmic-ray muon polarization near <ab:math xmlns:ab="http://www.w3.org/1998/Math/MathML" display="inline"><ab:mn>1</ab:mn><ab:mtext> </ab:mtext><ab:mtext> </ab:mtext><ab:mi>TeV</ab:mi><ab:mo>/</ab:mo><ab:mi>c</ab:mi></ab:math>. These measurement results are useful to improve atmospheric neutrino simulations. Published by the American Physical Society 2024

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Physical review. D/Physical review. D.
Published
2024-10-25
DOI
https://doi.org/10.1103/physrevd.110.082008
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Neutrino Physics Research
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article

Measurements of the charge ratio and polarization of cosmic-ray muons with the Super-Kamiokande detector

C. W. Walter, H. W. Sobel, R. Kaneshima, M. R. Vagins et al.
Physical review. D/Physical review. D.
Neutrino Physics Research
article

Measurements of the charge ratio and polarization of cosmic-ray muons with the Super-Kamiokande detector

C. W. Walter, H. W. Sobel, R. Kaneshima, M. R. Vagins, K. Martens, K. Nishijima, T. Ishizuka, K. Ieki, M. Lamoureux, L. Ludovici, T. Kinoshita, S. Moriyama, Y. Hino, D. Barrow, K. Choi, Y. Itow, M. Mori, K. Wada, J. L. Raaf, M. Ikeda, D. Marin, M. Scott, S. Shima, D. Hadley, T. Nakadaira, X. Li, Lorenzo Périssé, Y. Hayato, F Nakanishi, Z. Hu, T. Suganuma, S. Suzuki, L. Kneale, J. Łagoda, H. Menjo, G. Barr, H. Zhong, M. Nicholson, A. Ali, S. Yoshida, R. Matsumoto, K. Okumura, A. Yankelevich, M. Shinoki, Th. A. Mueller, T. Nakamura, K. Shimizu, Y. Maekawa, H. Sekiya, H. Shiba, Y. Noguchi, M Kawaue, K. Nakamura, Y. Kanemura, H. Okazawa, S. B. Kim, M. D. Thiesse, A. Tarrant, Poonam Mehta, G. T. Burton, Yusuke Takagi, S. Locke, R. Rogly, Benda Xu, B. Bodur, A. Giampaolo, M. Mattiazzi, S. Watanabe, J. S. Jang, Y. Ommura, F. Nova, Y. Oyama, A. K. Ichikawa, K. Hiraide, T. Nakaya, R. Akutsu, J. Yang, B. Zaldivar, B. S. Yang, N. Taniuchi, T Tada, Jun Hu, Eiichiro Watanabe, K. Hosokawa, J. Yoo, Y. Koshio, T. Tashiro, M. Nakahata, C. K. Jung, E. Kwon, A. Holin, A. Minamino, L. Wan, H. Ishino, L.F. Thompson, S. Nakayama, R. G. Park, S. Sakai, S. Zsoldos, Ll. Marti, S. Izumiyama, K. Abe, A. A. Sztuc, Pascal Paganini, C. Bronner, L. N. Machado, G. Pronost, F. Iacob, Wei Shi, J. M. McElwee, T. Yano, N. Iovine, X. Wang, T. Katori, V. Berardi, T. Hasegawa, Junfeng Feng, Y. Nakano, M. Kuze, Y. Takeuchi, M. O’Flaherty, N. Shigeta, P. de Perio, Y. Satou, R. Okazaki, I. Yu, S. Miki, N. J. Griskevich, T. Ishida, Y. S. Prabhu, J. Xia, V. Gousy-Leblanc, M. Jia, T. Tsukamoto, H. Kitagawa, N. F. Calabria, H. Ozaki, S. Sano, L. H. V. Anthony, K. Terada, T. Wester, K. Scholberg, A. Beauchêne, S. Samani, G. D. Megias, S. Cao, K. Nakagiri, J. Jiang, E. Kearns, A. Konaka, Hiroshi Itô, J. Migenda, R. M. Ramsden, K. Ninomiya, B. Zhang, Y. Kotsar, Y. Takemoto, G. Pintaudi, S. M. Lakshmi, M Mandal, Masayuki Harada, R. A. Wendell, R. Gaur, J. Bian, S. Han, Y. Suzuki, S. T. Wilson, M. B. Smy, C. Jesús-Valls, J. Gao, A. Eguchi, A. Langella, S. Jung, Y. Suzuki, Shaomin Chen, G. Collazuol, B. W. Pointon, S. J. Jenkins, N. Ospina, F. Di Lodovico, J. W. Seo, M. Yokoyama, Yumiko Yoshioka, Y. Nakajima, M. Shiozawa, Z. Xie, M. Miura, V.V. Tereshchenko, Y. Kataoka, L. Cook, M. Jakkapu, N. McCauley, Y. Fukuda, J. Hill, Y. Uchida, P. Fernández, M. Gonin, T. Kajita, J. F. Martin, N. W. Prouse, K. Sakashita, T. Sekiguchi, D. Wark, M. Posiadała-Zezula, T. Kobayashi, D. H. Moon, J. Zalipska, H. Tanaka, C. Yanagisawa, O. Drapier, S. H. Lee, A. Takenaka, L. Labarga, M. Hartz, Y. Nishimura, P. Mijakowski, L. Feng, A. De Souza Santos, S. B. Boyd, B. Jamieson, S. J. Jenkins, J. Kameda, E. Radicioni, K. M. Tsui, G. De Rosa, M. Friend, T. Yoshida, B. Quilain, A. Goldsack, T. Kikawa, R. Edwards, M. G. Catanesi, J. G. Learned, T. Towstego, B. Richards, S. Tairafune, M. Ishitsuka, Y. Kashiwagi, S. Amanai, M. J. Wilking, T. Tano, S. Mine, Tomoaki Tomiya, S. Fujita, Y. Sonoda, K. Okamoto, N. A. Bhuiyan, J. E. P. Fannon, A. Takeda, M. Malek, M. C. Jang, Volodymyr Takhistov, T. Matsubara, Keita Yamauchi
article en

Abstract

We present the results of the charge ratio (<a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mi>R</a:mi></a:math>) and polarization (<c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:msubsup><c:mi>P</c:mi><c:mn>0</c:mn><c:mi>μ</c:mi></c:msubsup></c:math>) measurements using decay electron events collected between September 2008 and June 2022 with the Super-Kamiokande detector. Because of its underground location and long operation, we are able to perform high-precision measurements by accumulating cosmic-ray muons. We measured the muon charge ratio to be <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"><e:mi>R</e:mi><e:mo>=</e:mo><e:mn>1.32</e:mn><e:mo>±</e:mo><e:mn>0.02</e:mn><e:mo stretchy="false">(</e:mo><e:mrow><e:mi>stat</e:mi></e:mrow><e:mo>+</e:mo><e:mrow><e:mi>syst</e:mi></e:mrow><e:mo stretchy="false">)</e:mo></e:math> at <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"><i:msub><i:mi>E</i:mi><i:mi>μ</i:mi></i:msub><i:mi>cos</i:mi><i:msub><i:mi>θ</i:mi><i:mtext>Zenith</i:mtext></i:msub><i:mo>=</i:mo><i:msubsup><i:mn>0.7</i:mn><i:mrow><i:mo>−</i:mo><i:mn>0.2</i:mn></i:mrow><i:mrow><i:mo>+</i:mo><i:mn>0.3</i:mn></i:mrow></i:msubsup><i:mtext> </i:mtext><i:mtext> </i:mtext><i:mi>TeV</i:mi></i:math>, where <k:math xmlns:k="http://www.w3.org/1998/Math/MathML" display="inline"><k:msub><k:mi>E</k:mi><k:mi>μ</k:mi></k:msub></k:math> is the muon energy and <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:msub><m:mi>θ</m:mi><m:mtext>Zenith</m:mtext></m:msub></m:math> is the zenith angle of incoming cosmic-ray muons. This result is consistent with the Honda flux model while indicating a tension with the <o:math xmlns:o="http://www.w3.org/1998/Math/MathML" display="inline"><o:mi>π</o:mi><o:mi>K</o:mi></o:math> model of <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"><q:mn>1.9</q:mn><q:mi>σ</q:mi></q:math>. We also measured the muon polarization at the production location to be <s:math xmlns:s="http://www.w3.org/1998/Math/MathML" display="inline"><s:mrow><s:msubsup><s:mrow><s:mi>P</s:mi></s:mrow><s:mrow><s:mn>0</s:mn></s:mrow><s:mrow><s:mi>μ</s:mi></s:mrow></s:msubsup><s:mo>=</s:mo><s:mn>0.52</s:mn><s:mo>±</s:mo><s:mn>0.02</s:mn><s:mtext> </s:mtext><s:mtext> </s:mtext><s:mo stretchy="false">(</s:mo><s:mrow><s:mi>stat</s:mi></s:mrow><s:mo>+</s:mo><s:mrow><s:mi>syst</s:mi></s:mrow><s:mo stretchy="false">)</s:mo></s:mrow></s:math> at the muon momentum of <w:math xmlns:w="http://www.w3.org/1998/Math/MathML" display="inline"><w:msubsup><w:mn>0.9</w:mn><w:mrow><w:mo>−</w:mo><w:mn>0.1</w:mn></w:mrow><w:mrow><w:mo>+</w:mo><w:mn>0.6</w:mn></w:mrow></w:msubsup><w:mtext> </w:mtext><w:mtext> </w:mtext><w:mi>TeV</w:mi><w:mo>/</w:mo><w:mi>c</w:mi></w:math> at the surface of the mountain; this also suggests a tension with the Honda flux model of <y:math xmlns:y="http://www.w3.org/1998/Math/MathML" display="inline"><y:mn>1.5</y:mn><y:mi>σ</y:mi></y:math>. This is the most precise measurement ever to experimentally determine the cosmic-ray muon polarization near <ab:math xmlns:ab="http://www.w3.org/1998/Math/MathML" display="inline"><ab:mn>1</ab:mn><ab:mtext> </ab:mtext><ab:mtext> </ab:mtext><ab:mi>TeV</ab:mi><ab:mo>/</ab:mo><ab:mi>c</ab:mi></ab:math>. These measurement results are useful to improve atmospheric neutrino simulations. Published by the American Physical Society 2024

Physical review. D/Physical review. D.Vol. 110(8)
Boston University (US), Chonnam National University (KR), Tokyo Institute of Technology (JP), California State University System (US), Rutherford Appleton Laboratory (GB), University of Minnesota (US), Tokai University (JP), State University of New York (US), University of Hawaii System (US), Okayama University of Science (JP), University of Padua (IT), High Energy Accelerator Research Organization (JP), Seoul National University (KR), University of Liverpool (GB), Miyagi University of Education (JP), Tokyo University of Science (JP), Okayama University (JP), Kavli Institute for the Physics and Mathematics of the Universe (JP), Duke University (US), British Columbia Institute of Technology (CA), Yokohama National University (JP), King's College London (GB), University of Toronto (CA), Osaka Electro-Communication University (JP), Tohoku University (JP), Keio University (JP), University of California, Irvine (US), Kyoto University (JP), University of Minnesota System (US), Daresbury Laboratory (GB), California State University, Dominguez Hills (US), Gwangju Institute of Science and Technology (KR), University of Warwick (GB), University of Oxford (GB), Chonnam National University Hospital (KR), National Centre for Nuclear Research (PL), Institute for Basic Science (KR), Istituto Nazionale di Fisica Nucleare, Sezione di Padova (IT), Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (IT), Istituto Nazionale di Fisica Nucleare, Sezione di Bari (IT), International Centre for Interdisciplinary Science and Education (VN), Laboratoire Leprince-Ringuet (FR), Shizuoka University of Welfare (JP), Istituto Nazionale di Fisica Nucleare, Sezione di Roma I (IT), Gifu University (JP), University of Toyama (JP), Institute for Cosmic Ray Research (JP), University of Warsaw (PL), Imperial College London (GB), Stony Brook University (US), Nagoya University (JP), Universidad Autónoma de Madrid (ES), Kobe University (JP), Polytechnic University of Bari (IT), The University of Tokyo (JP), University of Glasgow (GB), Sungkyunkwan University (KR), University of Silesia in Katowice (PL), The University of Winnipeg (CA), University of Sheffield (GB), Tsinghua University (CN)
National Science Foundation, U.S. Department of Energy, Compute Canada, Western Canada Research Grid, European Commission, National Research Foundation, Ministry of Education, Culture, Sports, Science and Technology, National Natural Science Foundation of China, Ministry of Education, Ministry of Science, ICT and Future Planning, National Research Foundation of Korea, Narodowe Centrum Nauki, Ministerstwo Edukacji i Nauki, Ministerio de Ciencia e Innovación, Institute for Basic Science, Horizon 2020 Framework Programme, Natural Sciences and Engineering Research Council of Canada, Science and Technology Facilities Council, Japan Society for the Promotion of Science, HORIZON EUROPE Marie Sklodowska-Curie Actions
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Neutrino Physics Research
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