1. Low-energy astrophysics with KamLAND
- Author
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Tomomi Gima, Thomas O'Donnell, Azusa Gando, Masashi Yoshida, Takahiko Hachiya, Hiroto Sambonsugi, Masayuki Koga, Atsuto Takeuchi, Yoshiki Wada, Naoya Maemura, John Gregory Learned, K. Ueshima, Sei Ieki, Shingo Hayashida, Sanshiro Enomoto, Yasuhiro Takemoto, Haruhiko Miyake, Kunio Inoue, Chistopher Grant, Dmitry Chernyak, Tadao Mitsui, Shuhei Obara, Junpei Shirai, Jason A. Detwiler, Alexandre Kozlov, Keishi Hosokawa, Yuki Yoshida, Zhenghao Fu, Rikuo Nakamura, K. Tamae, Hiroko Watanabe, Kosuke Nakamura, Kazuhiro Nakamura, Seisho Abe, Anna Goto, Kazumi Hata, Hugon J Karwowski, Yuya Suzuki, Yuto Kamei, Nanami Kawada, Yuri Efremenko, Yoshihito Gando, Itaru Shimizu, Kensuke Shiraishi, Brian Kurt Fujikawa, Stefano Dell'Oro, Taichi Sakai, Haruo Ikeda, Jelena Maricic, Bruce Edmond Berger, Tatsuya Kinoshita, Werner Tornow, Koichi Ichimura, Koji Ishidoshiro, Patric Decowski, Jonathan Ouellet, Spencer N. Axani, Atsuko Ichikawa, Sei Yoshida, Yasuhiro Kishimoto, A. Suzuki, Lindley Winslow, Sachihiro Asami, Aobo Li, Saori Umehara, Dian M. Markoff, Ken-Ichi Fushimi, H. Ozaki, Kengo Nakamura, and XENON (IHEF, IoP, FNWI)
- Subjects
Physics ,Nuclear physics ,Low energy - Abstract
We present two results of a search for MeV-scale neutrino and anti-neutrino events correlated with gravitational wave events/candidates and large solar flares with KamLAND. The KamLAND detector is a large-volume neutrino detector using liquid scintillator, which is located at 1 km underground under the top of Mt. Ikenoyama in Kamioka, Japan. KamLAND has multiple reaction channels to detect neutrinos. Electron antineutrino can be detected via inverse-beta decay with 1.8 MeV neutrino energy threshold. All flavors of neutrinos can be detected via neutrino-electron scattering without neutrino energy threshold. KamLAND has continued the neutrino observation since 2002 March. We use the data set of 60 gravitational waves provided by the LIGO/Virgo collaboration during their second and third observing runs and search for coincident electron antineutrino events in KamLAND. We find no significant coincident signals within a ±500 s timing window from each gravitational wave and present 90% C.L. upper limits on the electron antineutrino fluence between 108–1013 cm−2 for neutrino energies of 1.8–111 MeV. For a solar-flare neutrino search at KamLAND, we determine the timing window using the solar X-ray data set provided by the GOES satellite series from 2002 to 2019 and search for the excess of coincident event rate on the all-flavor neutrinos. We find no significant event rate excess in the flare time windows and get 90% C.L. upper limits on the fluence of neutrinos of all flavors (electron anti-neutrinos) between 1010–1013 cm−2 (108–1013 cm−2) for neutrino energies in the energy range of 0.4–35 MeV.
- Published
- 2021