Physics Letters B (Aug 2019)
Search for sub-GeV dark matter by annual modulation using XMASS-I detector
- M. Kobayashi,
- K. Abe,
- K. Hiraide,
- K. Ichimura,
- Y. Kishimoto,
- K. Kobayashi,
- S. Moriyama,
- M. Nakahata,
- H. Ogawa,
- K. Sato,
- H. Sekiya,
- T. Suzuki,
- A. Takeda,
- S. Tasaka,
- M. Yamashita,
- B.S. Yang,
- N.Y. Kim,
- Y.D. Kim,
- Y. Itow,
- K. Kanzawa,
- K. Masuda,
- K. Martens,
- Y. Suzuki,
- B.D. Xu,
- K. Miuchi,
- N. Oka,
- Y. Takeuchi,
- Y.H. Kim,
- K.B. Lee,
- M.K. Lee,
- Y. Fukuda,
- M. Miyasaka,
- K. Nishijima,
- K. Fushimi,
- G. Kanzaki,
- S. Nakamura
Affiliations
- M. Kobayashi
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan
- K. Abe
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- K. Hiraide
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- K. Ichimura
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- Y. Kishimoto
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- K. Kobayashi
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- S. Moriyama
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- M. Nakahata
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- H. Ogawa
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- K. Sato
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan
- H. Sekiya
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- T. Suzuki
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan
- A. Takeda
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- S. Tasaka
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan
- M. Yamashita
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- B.S. Yang
- Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- N.Y. Kim
- Center for Underground Physics, Institute for Basic Science, 70 Yuseong-daero 1689-gil, Yuseong-gu, Daejeon, 305-811, South Korea
- Y.D. Kim
- Center for Underground Physics, Institute for Basic Science, 70 Yuseong-daero 1689-gil, Yuseong-gu, Daejeon, 305-811, South Korea
- Y. Itow
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Aichi 464-8601, Japan; Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8602, Japan
- K. Kanzawa
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Aichi 464-8601, Japan
- K. Masuda
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Aichi 464-8601, Japan
- K. Martens
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- Y. Suzuki
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- B.D. Xu
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- K. Miuchi
- Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan
- N. Oka
- Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan
- Y. Takeuchi
- Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
- Y.H. Kim
- Korea Research Institute of Standards and Science, Daejeon 305-340, South Korea; Center for Underground Physics, Institute for Basic Science, 70 Yuseong-daero 1689-gil, Yuseong-gu, Daejeon, 305-811, South Korea
- K.B. Lee
- Korea Research Institute of Standards and Science, Daejeon 305-340, South Korea
- M.K. Lee
- Korea Research Institute of Standards and Science, Daejeon 305-340, South Korea
- Y. Fukuda
- Department of Physics, Miyagi University of Education, Sendai, Miyagi 980-0845, Japan
- M. Miyasaka
- Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan
- K. Nishijima
- Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan
- K. Fushimi
- Department of Physics, Tokushima University, 1-1 Minami Josanjimacho Tokushima city, Tokushima, 770-8506, Japan
- G. Kanzaki
- Department of Physics, Tokushima University, 1-1 Minami Josanjimacho Tokushima city, Tokushima, 770-8506, Japan
- S. Nakamura
- Department of Physics, Faculty of Engineering, Yokohama National University, Yokohama, Kanagawa 240-8501, Japan
- Journal volume & issue
-
Vol. 795
pp. 308 – 313
Abstract
A search for dark matter (DM) with mass in the sub-GeV region (0.32–1 GeV) was conducted by looking for an annual modulation signal in XMASS, a single-phase liquid xenon detector. Inelastic nuclear scattering accompanied by bremsstrahlung emission was used to search down to an electron equivalent energy of 1 keV. The data used had a live time of 2.8 years (3.5 years in calendar time), resulting in a total exposure of 2.38 ton-years. No significant modulation signal was observed and 90% confidence level upper limits of 1.6×10−33 cm2 at 0.5 GeV was set for the DM-nucleon cross section. This is the first experimental result of a search for DM mediated by the bremsstrahlung effect. In addition, a search for DM with mass in the multi-GeV region (4–20 GeV) was conducted with a lower energy threshold than previous analysis of XMASS. Elastic nuclear scattering was used to search down to a nuclear recoil equivalent energy of 2.3 keV, and upper limits of 2.9 ×10−42 cm2 at 8 GeV was obtained. Keywords: Sub-GeV dark matter, Annual modulation, Liquid xenon
