Search for light WIMP captured in the Sun using contained events in Super-Kamiokande

THE SUPER-KAMIOKANDE COLLABORATION

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Abstract

Super-Kamiokande can search for dark matter by detecting neutrinos and muons which are produced by WIMP pair annihilations occur inside the Sun. The huge gravity and hydrogen-rich composition of the Sun combined with high sensitivity of Super-Kamiokande for low energy(few GeV) neutrinos allow us good sensitivity to light(few GeV to few 10 GeV) WIMP dark matter, especially for spin-dependent coupling case. In this analysis, we increased signal acceptance by using fully-contained and partially-contained neutrino events added to up-going muons in Super-Kamiokande. We also used minimum χ 2 method to use energy, direction and flavor informations. We fitted Super-Kamiokande I-IV data to find the allowed contribution of WIMP-induced neutrino events added to large back-ground of atmospheric neutrino events. As a result, we found no signal observed and the null result was interpreted as upper limit on the spin-dependent (SD) WIMP-proton elastic scattering cross-section for χχ → bb ¯ and χχ → τ + τ WIMP annihilation channels. We set current best limit for WIMP mass below 100 GeV.

Original languageEnglish
Title of host publicationProceedings of the 33rd International Cosmic Rays Conference, ICRC 2013
PublisherSociedade Brasileira de Fisica
ISBN (Electronic)9788589064293
Publication statusPublished - 2013 Jan 1
Externally publishedYes
Event33rd International Cosmic Rays Conference, ICRC 2013 - Rio de Janeiro, Brazil
Duration: 2013 Jul 22013 Jul 9

Publication series

NameProceedings of the 33rd International Cosmic Rays Conference, ICRC 2013
Volume2013-October

Conference

Conference33rd International Cosmic Rays Conference, ICRC 2013
CountryBrazil
CityRio de Janeiro
Period13/7/213/7/9

Fingerprint

weakly interacting massive particles
sun
neutrinos
muons
dark matter
sensitivity
proton scattering
acceptability
scattering cross sections
elastic scattering
gravitation
energy
hydrogen

Keywords

  • Indirect WIMP search
  • Super-Kamiokande

ASJC Scopus subject areas

  • Nuclear and High Energy Physics

Cite this

THE SUPER-KAMIOKANDE COLLABORATION (2013). Search for light WIMP captured in the Sun using contained events in Super-Kamiokande. In Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013 (Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013; Vol. 2013-October). Sociedade Brasileira de Fisica.

Search for light WIMP captured in the Sun using contained events in Super-Kamiokande. / THE SUPER-KAMIOKANDE COLLABORATION.

Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013. Sociedade Brasileira de Fisica, 2013. (Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013; Vol. 2013-October).

Research output: Chapter in Book/Report/Conference proceedingConference contribution

THE SUPER-KAMIOKANDE COLLABORATION 2013, Search for light WIMP captured in the Sun using contained events in Super-Kamiokande. in Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013. Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013, vol. 2013-October, Sociedade Brasileira de Fisica, 33rd International Cosmic Rays Conference, ICRC 2013, Rio de Janeiro, Brazil, 13/7/2.
THE SUPER-KAMIOKANDE COLLABORATION. Search for light WIMP captured in the Sun using contained events in Super-Kamiokande. In Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013. Sociedade Brasileira de Fisica. 2013. (Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013).
THE SUPER-KAMIOKANDE COLLABORATION. / Search for light WIMP captured in the Sun using contained events in Super-Kamiokande. Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013. Sociedade Brasileira de Fisica, 2013. (Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013).
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AU - Hayato, Y.

AU - Iyogi, K.

AU - Kameda, J.

AU - Kishimoto, Y.

AU - Miura, M.

AU - Moriyama, S.

AU - Nakahata, M.

AU - Nakano, Y.

AU - Nakayama, S.

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AU - Lee, K. P.

AU - Nishimura, Yasuhiro

AU - Okumura, K.

AU - McLachlan, T.

AU - Labarga, L.

AU - Kearns, E.

AU - Raaf, J. L.

AU - Stone, J. L.

AU - Sulak, L. R.

AU - Berkman, S.

AU - Tanaka, H. A.

AU - Tobayama, S.

AU - Goldhaber, M.

AU - Carminati, G.

AU - Kropp, W. R.

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AU - Renshaw, A.

AU - Smy, M. B.

AU - Sobel, H. W.

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AU - Kim, J. Y.

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AU - Scholberg, K.

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N2 - Super-Kamiokande can search for dark matter by detecting neutrinos and muons which are produced by WIMP pair annihilations occur inside the Sun. The huge gravity and hydrogen-rich composition of the Sun combined with high sensitivity of Super-Kamiokande for low energy(few GeV) neutrinos allow us good sensitivity to light(few GeV to few 10 GeV) WIMP dark matter, especially for spin-dependent coupling case. In this analysis, we increased signal acceptance by using fully-contained and partially-contained neutrino events added to up-going muons in Super-Kamiokande. We also used minimum χ 2 method to use energy, direction and flavor informations. We fitted Super-Kamiokande I-IV data to find the allowed contribution of WIMP-induced neutrino events added to large back-ground of atmospheric neutrino events. As a result, we found no signal observed and the null result was interpreted as upper limit on the spin-dependent (SD) WIMP-proton elastic scattering cross-section for χχ → bb ¯ and χχ → τ + τ − WIMP annihilation channels. We set current best limit for WIMP mass below 100 GeV.

AB - Super-Kamiokande can search for dark matter by detecting neutrinos and muons which are produced by WIMP pair annihilations occur inside the Sun. The huge gravity and hydrogen-rich composition of the Sun combined with high sensitivity of Super-Kamiokande for low energy(few GeV) neutrinos allow us good sensitivity to light(few GeV to few 10 GeV) WIMP dark matter, especially for spin-dependent coupling case. In this analysis, we increased signal acceptance by using fully-contained and partially-contained neutrino events added to up-going muons in Super-Kamiokande. We also used minimum χ 2 method to use energy, direction and flavor informations. We fitted Super-Kamiokande I-IV data to find the allowed contribution of WIMP-induced neutrino events added to large back-ground of atmospheric neutrino events. As a result, we found no signal observed and the null result was interpreted as upper limit on the spin-dependent (SD) WIMP-proton elastic scattering cross-section for χχ → bb ¯ and χχ → τ + τ − WIMP annihilation channels. We set current best limit for WIMP mass below 100 GeV.

KW - Indirect WIMP search

KW - Super-Kamiokande

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