Sensitivity of Super-Kamiokande with Gadolinium to Low Energy Anti-neutrinos from Pre-supernova Emission
C. Simpson, K. Abe, C. Bronner, Y. Hayato, M. Ikeda, H. Ito, K. Iyogi, J. Kameda, Y. Kataoka, Y. Kato, Y. Kishimoto, Ll. Marti, M. Miura, S. Moriyama, T. Mochiz… 展开作者
C. Simpson, K. Abe, C. Bronner, Y. Hayato, M. Ikeda, H. Ito, K. Iyogi, J. Kameda, Y. Kataoka, Y. Kato, Y. Kishimoto, Ll. Marti, M. Miura, S. Moriyama, T. Mochizuki, M. Nakahata, Y. Nakajima, S. Nakayama, T. Okada, K. Okamoto, A. Orii, G. Pronost, H. Sekiya, M. Shiozawa, Y. Sonoda, A. Takeda, A. Takenaka, H. Tanaka, T. Yano, R. Akutsu, T. Kajita, K. Okumura, R. Wang, J. Xia, D. Bravo-Berguño, L. Labarga, P. Fernandez, F. d. M. Blaszczyk, C. Kachulis, E. Kearns, J. L. Raaf, J. L. Stone, L. Wan, T. Wester, S. Sussman, S. Berkman, J. Bian, N. J. Griskevich, W. R. Kropp, S. Locke, S. Mine, M. B. Smy, H. W. Sobel, V. Takhistov, P. Weatherly, K. S. Ganezer, J. Hill, J. Y. Kim, I. T. Lim, R. G. Park, B. Bodur, K. Scholberg, C. W. Walter, A. Coffani, O. Drapier, M. Gonin, J. Imber, Th. A. Mueller, P. Paganini, T. Ishizuka, T. Nakamura, J. S. Jang, K. Choi, J. G. Learned, S. Matsuno, R. P. Litchfield, A. A. Sztuc, Y. Uchida, M. O. Wascko, V. Berardi, N. F. Calabria, M. G. Catanesi, R. A. Intonti, E. Radicioni, G. De Rosa, G. Collazuol, F. Iacob, L. Ludovici, Y. Nishimura, S. Cao, M. Friend, T. Hasegawa, T. Ishida, T. Kobayashi, T. Nakadaira, K. Nakamura, Y. Oyama, K. Sakashita, T. Sekiguchi, T. Tsukamoto, KE. Abe, M. Hasegawa, Y. Isobe, H. Miyabe, Y. Nakano, T. Shiozawa, T. Sugimoto, A. T. Suzuki, Y. Takeuchi, A. Ali, Y. Ashida, T. Hayashino, S. Hirota, M. Jiang, T. Kikawa, M. Mori, KE. Nakamura, T. Nakaya, R. A. Wendell, L. H. V. Anthony, N. McCauley, A. Pritchard, K. M. Tsui, Y. Fukuda, Y. Itow, M. Murrase, T. Niwa, M. Taani, M. Tsukada, P. Mijakowski, K. Frankiewicz, C. K. Jung, X. Li, J. L. Palomino, G. Santucci, C. Vilela, M. J. Wilking, C. Yanagisawa, D. Fukuda, M. Harada, K. Hagiwara, T. Horai, H. Ishino, S. Ito, Y. Koshio, M. Sakuda, Y. Takahira, C. Xu, Y. Kuno, L. Cook, D. Wark, F. Di Lodovico, S. Molina Sedgwick, B. Richards, S. Zsoldos, S. B. Kim, R. Tacik, M. Thiesse, L. Thompson, H. Okazawa, Y. Choi, K. Nishijima, M. Koshiba, M. Yokoyama, A. Goldsack, K. Martens, M. Murdoch, B. Quilain, Y. Suzuki, M. R. Vagins, M. Kuze, Y. Okajima, M. Tanaka, T. Yoshida, M. Ishitsuka, R. Matsumoto, K. Ohta, J. F. Martin, C. M. Nantais, H. A. Tanaka, T. Towstego, M. Hartz, A. Konaka, P. de Perio, S. Chen, B. Jamieson, J. Walker, A. Minamino, K. Okamoto, G. Pintaudi
Supernova detection is a major objective of the Super-Kamiokande (SK) experiment. In the next stage of SK (SK-Gd), gadolinium (Gd) sulfate will be added to the detector, which will improve the ability of the detector to identify neutrons. A core-collapse supernova will be preceded by an increasing flux of neutrinos and anti-neutrinos, from thermal and weak nuclear processes in the star, over a timescale of hours; some of which may be detected at SK-Gd. This could provide an early warning of an imminent core-collapse supernova, hours earlier than the detection of the neutrinos from core collapse. Electron anti-neutrino detection will rely on inverse beta decay events below the usual analysis energy threshold of SK, so Gd loading is vital to reduce backgrounds while maximising detection efficiency. Assuming normal neutrino mass ordering, more than 200 events could be detected in the final 12 hours before core collapse for a 15-25 solar mass star at around 200 pc, which is representative of the nearest red supergiant to Earth, $\mathrmα$Ori (Betelgeuse). At a statistical false alarm rate of 1 per century, detection could be up to 10 hours before core collapse, and a pre-supernova star could be detected by SK-Gd up to 600 pc away. A pre-supernova alert could be provided to the astrophysics community following gadolinium loading.
Okayama University（冈山大学）；Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo（东京大学宇宙射线研究所神冈观测站）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo（东京大学基础物理学与数学柯尔维特研究所（WPI））
Search for Diffuse Supernova Neutrino Background with 956.2 days of Super-Kamiokande Gadolinium Dataset
Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo（东京大学宇宙线研究所神冈观测站）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo（东京大学前沿研究院 Kavli宇宙物理学与数学研究所）
An axion constraint from the diffuse supernova neutrino background indicated by Super-Kamiokande
Keio University（庆应义塾大学）；National Astronomical Observatory of Japan（日本国立天文台）；The Graduate University for Advanced Studies (SOKENDAI)（综合研究大学院大学）；Department of Astronomy, The University of Tokyo（东京大学天文学系）；Theory Center, IPNS, KEK（高能加速器研究机构理论中心）；Kavli IPMU (WPI), The University of Tokyo（东京大学加瓦利宇宙起源研究前沿中心）；National Institute of Technology (KOSEN), Numazu College（静冈县立沼津工业高等专门学校）
Optical Follow-Up Strategies for the Next Neutrino-Detected Galactic Core-Collapse Supernova
Université Paris Cité, CNRS, Astroparticules et Cosmologie（巴黎西岱大学）；Aix Marseille Univ, CNRS/IN2P3, CPPM（艾克斯-马赛大学）；School of Physics and Astronomy, University of Minnesota（明尼苏达大学物理与天文学院）
Search for supernova bursts in Super-Kamiokande IV
Super-Kamiokande自1996年开始运行以来，一直在实时连续地搜索核心坍缩超新星的中微子爆发特征。目前的工作重点是探测更遥远的超新星，其事件率可能太小而无法实时触发，但可以使用离线方法进行识别。对2008年至2018年收集的数据进行分析，没有发现遥远超新星爆发的证据。这就建立了在90% C. L.时，100 kpc以内的核心坍缩超新星速率的上限为0.29年$^{-1}$。对于没有爆炸而直接坍缩成黑洞的超新星，极限达到300千秒差距。
