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arXiv:2312.12907hep-ex

Solar neutrino measurements using the full data period of Super-Kamiokande-IV

Super-Kamiokande Collaboration, :, K. Abe, C. Bronner, Y. Hayato, K. Hiraide, K. Hosokawa, K. Ieki, M. Ikeda, S. Imaizumi, K. Iyogi, J. Kameda, Y. Kanemura, R. Kaneshima, Y. Kashiwagi, Y. Kataoka, Y. Kato, Y. Kishimoto, S. Miki, S. Mine, M. Miura, T. Mochizuki, S. Moriyama, Y. Nagao, M. Nakahata, Y. Nakano, S. Nakayama, Y. Noguchi, T. Okada, K. Okamoto, A. Orii, K. Sato, H. Sekiya, H. Shiba, K. Shimizu, M. Shiozawa, Y. Sonoda, Y. Suzuki, A. Takeda, Y. Takemoto, A. Takenaka, H. Tanaka, S. Watanabe, T. Yano, S. Han, T. Kajita, K. Okumura, T. Tashiro, T. Tomiya, R. Wang, X. Wang, S. Yoshida, D. Bravo-Berguno, P. Fernandez, L. Labarga, N. Ospina, B. Zaldivar, B. W. Pointon, F. d. M. Blaszczyk, C. Kachulis, E. Kearns, J. L. Raaf, J. L. Stone, L. Wan, T. Wester, J. Bian, N. J. Griskevich, W. R. Kropp, S. Locke, M. B. Smy, H. W. Sobel, V. Takhistov, P. Weatherly, A. Yankelevich, K. S. Ganezer, J. Hill, M. C. Jang, J. Y. Kim, S. Lee, I. T. Lim, D. H. Moon, R. G. Park, B. Bodur, K. Scholberg, C. W. Walter, A. Beauchene, L. Bernard, A. Coffani, O. Drapier, S. El Hedri, A. Giampaolo, J. Imber, Th. A. Mueller, P. Paganini, R. Rogly, B. Quilain, A. Santos, T. Nakamura, J. S. Jang, L. N. Machado, J. G. Learned, S. Matsuno, N. Iovine, K. Choi, S. Cao, L. H. V. Anthony, R. P. Litchfield, N. Prouse, D. Marin, M. Scott, A. A. Sztuc, Y. Uchida, V. Berardi, M. G. Catanesi, R. A. Intonti, E. Radicioni, N. F. Calabria, G. De Rosa, A. Langella, G. Collazuol, F. Iacob, M. Lamoureux, M. Mattiazzi, L. Ludovici, M. Gonin, L. Perisse, G. Pronost, C. Fujisawa, Y. Maekawa, Y. Nishimura, R. Okazaki, M. Friend, T. Hasegawa, T. Ishida, M. Jakkapu, T. Kobayashi, T. Matsubara, T. Nakadaira, K. Nakamura, Y. Oyama, K. Sakashita, T. Sekiguchi, T. Tsukamoto, T. Boschi, N. Bhuiyan, G. T. Burton, J. Gao, A. Goldsack, T. Katori, F. Di Lodovico, J. Migenda, S. Molina Sedgwick, R. M. Ramsden, M. Taani, Z. Xie, S. Zsoldos, KE. Abe, M. Hasegawa, Y. Isobe, Y. Kotsar, H. Miyabe, H. Ozaki, T. Shiozawa, T. Sugimoto, A. T. Suzuki, Y. Takagi, Y. Takeuchi, S. Yamamoto, H. Zhong, Y. Ashida, J. Feng, L. Feng, T. Hayashino, S. Hirota, J. R. Hu, Z. Hu, M. Jiang, M. Kawaue, T. Kikawa, M. Mori, KE. Nakamura, T. Nakaya, R. A. Wendell, K. Yasutome, S. J. Jenkins, N. McCauley, P. Mehta, A. Pritchard, A. Tarrant, M. J. Wilking, Y. Fukuda, Y. Itow, H. Menjo, M. Murase, K. Ninomiya, T. Niwa, M. Tsukada, Y. Yoshioka, K. Frankiewicz, J. Lagoda, M. Mandal, P. Mijakowski, Y. S. Prabhu, J. Zalipska, J. Jiang, M. Jia, C. K. Jung, J. L. Palomino, G. Santucci, W. Shi, C. Vilela, C. Yanagisawa, D. Fukuda, K. Hagiwara, M. Harada, Y. Hino, T. Horai, H. Ishino, S. Ito, H. Kitagawa, Y. Koshio, W. Ma, F. Nakanishi, N. Piplani, S. Sakai, M. Sakuda, T. Tada, T. Tano, C. Xu, R. Yamaguchi, T. Ishizuka, Y. Kuno, G. Barr, D. Barrow, L. Cook, S. Samani, C. Simpson, D. Wark, A. M. Holin, F. Nova, S. Jung, B. Yang, J. Y. Yang, J. Yoo, J. E. P. Fannon, L. Kneale, M. Malek, J. M. McElwee, O. Stone, M. D. Thiesse, L. F. Thompson, S. T. Wilson, H. Okazawa, S. M. Lakshmi, Y. Choi, S. B. Kim, E. Kwon, J. W. Seo, I. Yu, A. K. Ichikawa, K. Nakamura, S. Tairahune, K. Nishijima, A. Eguchi, K. Iwamoto, K. Nakagiri, Y. Nakajima, N. Ogawa, S. Shima, E. Watanabe, M. Yokoyama, R. G. Calland, S. Fujita, C. Jesus-Valls, X. Junjie, T. K. Ming, P. de Perio, K. Martens, M. Murdoch, M. R. Vagins, S. Izumiyama, M. Kuze, R. Matsumoto, Y. Okajima, M. Tanaka, T. Yoshida, M. Inomoto, M. Ishitsuka, H. Ito, T. Kinoshita, R. Matsumoto, K. Ohta, Y. Ommura, M. Shinoki, N. Shigeta, T. Suganuma, K. Yamaguchi, T. Yoshida, J. F. Martin, C. M. Nantais, H. A. Tanaka, T. Towstego, R. Gaur, V. Gousy-Leblanc, M. Hartz, A. Konaka, X. Li, S. Chen, B. D. Xu, B. Zhang, S. Berkman, M. Posiadala-Zezula, S. B. Boyd, R. Edwards, D. Hadley, M. Nicholson, M. O'Flaherty, B. Richards, A. Ali, B. Jamieson, J. Walker, S. Amanai, Ll. Marti, A. Minamino, K. Okamoto, G. Pintaudi, S. Sano, R. Sasaki, S. Suzuki, K. Wada

Abstract

An analysis of solar neutrino data from the fourth phase of Super-Kamiokande~(SK-IV) from October 2008 to May 2018 is performed and the results are presented. The observation time of the data set of SK-IV corresponds to $2970$~days and the total live time for all four phases is $5805$~days. For more precise solar neutrino measurements, several improvements are applied in this analysis: lowering the data acquisition threshold in May 2015, further reduction of the spallation background using neutron clustering events, precise energy reconstruction considering the time variation of the PMT gain. The observed number of solar neutrino events in $3.49$--$19.49$ MeV electron kinetic energy region during SK-IV is $65,443^{+390}_{-388}\,(\mathrm{stat.})\pm 925\,(\mathrm{syst.})$ events. Corresponding $\mathrm{^{8}B}$ solar neutrino flux is $(2.314 \pm 0.014\, \rm{(stat.)} \pm 0.040 \, \rm{(syst.)}) \times 10^{6}~\mathrm{cm^{-2}\,s^{-1}}$, assuming a pure electron-neutrino flavor component without neutrino oscillations. The flux combined with all SK phases up to SK-IV is $(2.336 \pm 0.011\, \rm{(stat.)} \pm 0.043 \, \rm{(syst.)}) \times 10^{6}~\mathrm{cm^{-2}\,s^{-1}}$. Based on the neutrino oscillation analysis from all solar experiments, including the SK $5805$~days data set, the best-fit neutrino oscillation parameters are $\rm{sin^{2} θ_{12,\,solar}} = 0.306 \pm 0.013 $ and $Δm^{2}_{21,\,\mathrm{solar}} = (6.10^{+ 0.95}_{-0.81}) \times 10^{-5}~\rm{eV}^{2}$, with a deviation of about 1.5$σ$ from the $Δm^{2}_{21}$ parameter obtained by KamLAND. The best-fit neutrino oscillation parameters obtained from all solar experiments and KamLAND are $\sin^{2} θ_{12,\,\mathrm{global}} = 0.307 \pm 0.012 $ and $Δm^{2}_{21,\,\mathrm{global}} = (7.50^{+ 0.19}_{-0.18}) \times 10^{-5}~\rm{eV}^{2}$.

arXiv comments
47 pages, 61 figures
Journal reference
Phys. Rev. D 109, 092001 (2024)
DOI
doi:10.1103/PhysRevD.109.092001
Subjects
hep-exHigh Energy Physics, Experiment

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  1. ArXiv now offers papers in HTML format 2 comments

    • doesn't work great with long author lists... https://browse.arxiv.org/html/2312.12907v1

      cozzydView on HNParent context

    • The PDF is worse, so there is no simple answer to this: https://arxiv.org/pdf/2312.12907v1.pdf At least the HTML version pairs each author with their affiliations, instead of the PDF which has all the names on page 1, and all the affiliations on page 2. That's completely…

      degenerateView on HNParent context

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