Search for sub-GeV dark matter by annual modulation using XMASS-I detector
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 en...
| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
| Published: |
Elsevier
2019-08-01
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| Series: | Physics Letters B |
| Online Access: | http://www.sciencedirect.com/science/article/pii/S0370269319304009 |
| _version_ | 1818297124936220672 |
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| author | 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 |
| author_facet | 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 |
| author_sort | M. Kobayashi |
| collection | DOAJ |
| description | 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 |
| first_indexed | 2024-12-13T04:14:27Z |
| format | Article |
| id | doaj.art-aaaf271fe5994e20863570f903b00227 |
| institution | Directory Open Access Journal |
| issn | 0370-2693 |
| language | English |
| last_indexed | 2024-12-13T04:14:27Z |
| publishDate | 2019-08-01 |
| publisher | Elsevier |
| record_format | Article |
| series | Physics Letters B |
| spelling | doaj.art-aaaf271fe5994e20863570f903b002272022-12-21T23:59:56ZengElsevierPhysics Letters B0370-26932019-08-01795308313Search for sub-GeV dark matter by annual modulation using XMASS-I detectorM. Kobayashi0K. Abe1K. Hiraide2K. Ichimura3Y. Kishimoto4K. Kobayashi5S. Moriyama6M. Nakahata7H. Ogawa8K. Sato9H. Sekiya10T. Suzuki11A. Takeda12S. Tasaka13M. Yamashita14B.S. Yang15N.Y. Kim16Y.D. Kim17Y. Itow18K. Kanzawa19K. Masuda20K. Martens21Y. Suzuki22B.D. Xu23K. Miuchi24N. Oka25Y. Takeuchi26Y.H. Kim27K.B. Lee28M.K. Lee29Y. Fukuda30M. Miyasaka31K. Nishijima32K. Fushimi33G. Kanzaki34S. Nakamura35Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, JapanKamioka 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, JapanKamioka 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, JapanKamioka 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, JapanKamioka 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, JapanKamioka 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, JapanKamioka 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, JapanKamioka 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, JapanKamioka 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, JapanKamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, JapanKamioka 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, JapanKamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, JapanKamioka 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, JapanKamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, JapanKamioka 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, JapanKamioka 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, JapanCenter for Underground Physics, Institute for Basic Science, 70 Yuseong-daero 1689-gil, Yuseong-gu, Daejeon, 305-811, South KoreaCenter for Underground Physics, Institute for Basic Science, 70 Yuseong-daero 1689-gil, Yuseong-gu, Daejeon, 305-811, South KoreaInstitute 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, JapanInstitute for Space-Earth Environmental Research, Nagoya University, Nagoya, Aichi 464-8601, JapanInstitute for Space-Earth Environmental Research, Nagoya University, Nagoya, Aichi 464-8601, JapanKavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, JapanKavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, JapanKavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, JapanDepartment of Physics, Kobe University, Kobe, Hyogo 657-8501, JapanDepartment of Physics, Kobe University, Kobe, Hyogo 657-8501, JapanDepartment 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, JapanKorea 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 KoreaKorea Research Institute of Standards and Science, Daejeon 305-340, South KoreaKorea Research Institute of Standards and Science, Daejeon 305-340, South KoreaDepartment of Physics, Miyagi University of Education, Sendai, Miyagi 980-0845, JapanDepartment of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, JapanDepartment of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, JapanDepartment of Physics, Tokushima University, 1-1 Minami Josanjimacho Tokushima city, Tokushima, 770-8506, JapanDepartment of Physics, Tokushima University, 1-1 Minami Josanjimacho Tokushima city, Tokushima, 770-8506, JapanDepartment of Physics, Faculty of Engineering, Yokohama National University, Yokohama, Kanagawa 240-8501, JapanA 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 xenonhttp://www.sciencedirect.com/science/article/pii/S0370269319304009 |
| spellingShingle | 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 Search for sub-GeV dark matter by annual modulation using XMASS-I detector Physics Letters B |
| title | Search for sub-GeV dark matter by annual modulation using XMASS-I detector |
| title_full | Search for sub-GeV dark matter by annual modulation using XMASS-I detector |
| title_fullStr | Search for sub-GeV dark matter by annual modulation using XMASS-I detector |
| title_full_unstemmed | Search for sub-GeV dark matter by annual modulation using XMASS-I detector |
| title_short | Search for sub-GeV dark matter by annual modulation using XMASS-I detector |
| title_sort | search for sub gev dark matter by annual modulation using xmass i detector |
| url | http://www.sciencedirect.com/science/article/pii/S0370269319304009 |
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