Publisher's Note: Search for dark matter WIMPs using upward through-going muons in Super-Kamiokande [Phys. Rev. D<b>70</b>, 083523 (2004)]

Desai, S.; Ashie, Y.; Fukuda, Seisuke; Fukuda, Y.; Ishihara, K.; Itow, Y.; Koshio, Y.; Minamino, A.; Miura, M.; Moriyama, S.; Nakahata, M.; Namba, T.; Nambu, R.; Obayashi, Y.; Sakurai, N.; Shiozawa, M.; Suzuki, Y.; Takeuchi, Hideki; Takeuchi, Y.; Yamada, Shuho; Ishitsuka, M.; Kajita, T.; Kaneyuki, K.; Nakayama, S.; Okada, Atsushi; Ooyabu, T.; Saji, C.; Earl, M.; Kearns, E.; Stone, J. L.; Sulak, L.; Walter, Christopher W.; Wang, W.; Goldhaber, M.; Barszczak, T.; Casper, D.; Cravens, J. P.; Gajewski, W.; Kropp, W. R.; Mine, S.; Liu, D. W.; Smy, M. B.; Sobel, H. W.; Sterner, C. W.; Vagins, M. R.; Ganezer, K. S.; Hill, J.; Keig, W. E.; Kim, J. Y.; Lim, I. T.; Ellsworth, R. W.; Tasaka, S.; Guillian, G.; Kibayashi, A.; Learned, J. G.; Matsuno, S.; Takemori, D.; Messier, M. D.; Hayato, Y.; Ichikawa, A. K.; Ishida, Toru; Ishii, T.; Iwashita, T.; Kameda, J.; Kobayashi, T.; Maruyama, T.; Nakamura, K.; Nitta, K.; Oyama, Y.; Sakuda, M.; Totsuka, Y.; Hasegawa, M.; Hayashi, Kenji; Inagaki, T.; Kato, I.; Maesaka, H.; Morita, T.; Nakaya, T.; Nishikawa, K.; Sasaki, T.; Ueda, S.; Yamamoto, S.; Haines, T. J.; Dazeley, S.; Hatakeyama, S.; Svoboda, R.; Blaufuss, E.; Goodman, J. A.; Sullivan, G. W.; Turčan, D.; Scholberg, K.; Habig, A.; Jung, C. K.; Kato, T.; Kobayashi, Kazuyoshi; Malek, M.; Mauger, C.; McGrew, C.; Sarrat, A.; Sharkey, E.; Yanagisawa, C.; Toshito, T.; Mitsuda, C.; Miyano, K.; Shibata, Tadashi; Kajiyama, Yuji; Nagashima, Y.; Takita, M.; Yoshida, Masato; Kim, H. I.; Kim, S. B.; Yoo, Juhyun; Okazawa, H.; Ishizuka, T.; Choi, Y.; Seo, H.; Gando, Y.; Hasegawa, T.; Inoue, K.; Shirai, J.; Suzuki, A.; Koshiba, M.; Hashimoto, Tsuyoshi; Nakajima, Yasuhiro; Nishijima, Kazuhiko; Harada, Takaaki; Ishino, H.; Morii, M.; Nishimura, Ryouhei; Watanabe, Y.; Kiełczewska, D.; Zalipska, J.; Gran, R.; Shiraishi, Kiyoshi; Washburn, K.; Wilkes, R. J.

doi:10.1103/physrevd.70.109901

Cited by 118 publications

(145 citation statements)

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“…The most significant of these constraints arise from the capture and subsequent annihilation of dark matter into neutrinos. These are then constrained by measurements at SuperKamiokande [44,[46][47][48]. Similarly, it has also been pointed out that the capture of dark matter in white dwarfs located in globular clusters with dark matter densities greater than $1000 times the mean Galactic dark matter density could also place limits on the dark matter-nucleon interaction cross section [49,50].…”

Section: Neutrino Detectorsmentioning

confidence: 97%

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Luminous dark matter

Feldstein

Graham²,

Rajendran³

2010

Phys. Rev. D

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We propose a dark matter model in which the signal in direct detection experiments arises from electromagnetic, not nuclear, energy deposition. This can provide a novel explanation for the DAMA result while avoiding many direct detection constraints. The dark matter state is taken nearly degenerate with another state. These states are naturally connected by a dipole moment operator, which can give both the dominant scattering and decay modes between the two states. The signal at DAMA then arises from dark matter scattering in the Earth into the excited state and decaying back to the ground state through emission of a single photon in the detector. This model has unique signatures in direct detection experiments. The density and chemical composition of the detector is irrelevant-only the total volume affects the event rate. In addition, the spectrum is a monoenergetic line, which can fit the DAMA signal well. This model is readily testable at experiments such as CDMS and XENON100 if they analyze their low-energy, electronic recoil events.

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Section: Neutrino Detectorsmentioning

confidence: 97%

“…Neutrino detectors like Borexino [43] and SuperKamiokande [44] are large volume detectors. However, their operating thresholds are close to $1 MeV and hence these experiments are insensitive to luminous dark matter.…”

Section: Neutrino Detectorsmentioning

confidence: 99%

Luminous dark matter

Feldstein

Graham²,

Rajendran³

2010

Phys. Rev. D

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“…These annihilations may produce high-energy neutrinos that escape the Sun. The Super-Kamiokande experiment places limits on such a neutrino flux [52]. Neutrinos may be produced either as the direct products of dark matter annihilations or through the decays of bottoms, charms, or taus produced in the annihilations.…”

Section: A Annihilation In the Sunmentioning

confidence: 99%

Exothermic dark matter

et al. 2010

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We propose a novel mechanism for dark matter to explain the observed annual modulation signal at DAMA/LIBRA which avoids existing constraints from every other dark matter direct detection experiment including CRESST, CDMS, and XENON10. The dark matter consists of at least two light states with mass $few GeV and splittings $5 keV. It is natural for the heavier states to be cosmologically long-lived and to make up an Oð1Þ fraction of the dark matter. Direct detection rates are dominated by the exothermic reactions in which an excited dark matter state downscatters off of a nucleus, becoming a lower energy state. In contrast to (endothermic) inelastic dark matter, the most sensitive experiments for exothermic dark matter are those with light nuclei and low threshold energies. Interestingly, this model can also naturally account for the observed low-energy events at CoGeNT. The only significant constraint on the model arises from the DAMA/LIBRA unmodulated spectrum but it can be tested in the near future by a low-threshold analysis of CDMS-Si and possibly other experiments including CRESST, COUPP, and XENON100.

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“…The parameter space above the dotted line is excluded at 90% C.L. by Super Kamiokande observations toward the direction of the Galactic center with a cone half angle of 5 [29].…”

Section: Resultsmentioning

confidence: 99%

“…Final states including 's or 's of dark matter not lighter than 1 TeV fit the PAMELA, HESS, and Fermi data best [28]. These leptophilic dark matter candidates [24] would copiously produce neutrinos [19] whose fluxes are constrained by the observations of Super Kamiokande [29] toward the direction of the Galactic center. Neutrinos with energies of the order of the dark matter mass, E m , would propagate without being deflected toward the Earth.…”

Section: Introductionmentioning

confidence: 90%

Muon fluxes and showers from dark matter annihilation in the Galactic center

et al. 2010

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We calculate contained and upward muon flux and contained shower event rates from neutrino interactions, when neutrinos are produced from annihilation of the dark matter in the Galactic center. We consider model-independent direct neutrino production and secondary neutrino production from the decay of taus, W bosons, and bottom quarks produced in the annihilation of dark matter. We illustrate how muon flux from dark matter annihilation has a very different shape than the muon flux from atmospheric neutrinos. We also discuss the dependence of the muon fluxes on the dark matter density profile and on the dark matter mass and of the total muon rates on the detector threshold. We consider both the upward muon flux, when muons are created in the rock below the detector, and the contained flux when muons are created in the (ice) detector. We also calculate the event rates for showers from neutrino interactions in the detector and show that the signal dominates over the background for 150 GeV < m < 1 TeV for E th sh ¼

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Publisher's Note: Search for dark matter WIMPs using upward through-going muons in Super-Kamiokande [Phys. Rev. D70, 083523 (2004)]

Cited by 118 publications

References 0 publications

Luminous dark matter

Luminous dark matter

Exothermic dark matter

Muon fluxes and showers from dark matter annihilation in the Galactic center

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