Search for dark matter WIMPs using upward through-going muons in Super-Kamiokande

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, S.; Ishitsuka, M.; Kajita, T.; Kaneyuki, K.; Nakayama, S.; Okada, Atsushi; Ooyabu, T.; Saji, C.; Earl, M.; Kearns, E.; Stone, J. L.; Sulak, L.; Walter, C. 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, Shuji; 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, Takashi; 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, J.; 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, K.; 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.70.083523

Cited by 269 publications

(159 citation statements)

References 66 publications

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“…The current experimental upper limits [48,49,50,51] from direct searches, assuming a default value of 0.3 GeV/cm 3 for the local DM density, as well as an indirect limit from neutralino annihilations into neutrinos in the Sun, the Earth or the Galactic center [52], which have also been shown in fig. 13, still remain a few order of magnitude above the predictions of the CMSSM.…”

Section: Implications For Direct Detection Of Dark Mattermentioning

confidence: 96%

Implications for the Constrained MSSM from a new prediction forb→sγ

Roszkowski

Austri²,

Trotta

2007

J. High Energy Phys.

151

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Abstract:We re-examine the properties of the Constrained MSSM in light of updated constraints, paying particular attention to the impact of the recent substantial shift in the Standard Model prediction for BR(B → X s γ). With the help of a Markov Chain Monte Carlo scanning technique, we vary all relevant parameters simultaneously and derive Bayesian posterior probability maps. We find that the case of µ > 0 remains favored, and that for µ < 0 it is considerably more difficult to find a good global fit to current constraints. In both cases we find a strong preference for a focus point region. This leads to improved prospects for detecting neutralino dark matter in direct searches, while superpartner searches at the LHC become more problematic, especially when µ < 0. In contrast, prospects for exploring the whole mass range of the lightest Higgs boson at the Tevatron and the LHC remain very good, which should, along with dark matter searches, allow one to gain access to the otherwise experimentally challenging focus point region. An alternative measure of the mean quality-of-fit which we also employ implies that present data are not yet constraining enough to draw more definite conclusions. We also comment on the dependence of our results on the choice of priors and on some other assumptions.

show abstract

Section: Implications For Direct Detection Of Dark Mattermentioning

confidence: 96%

Implications for the Constrained MSSM from a new prediction forb→sγ

Roszkowski

Austri²,

Trotta

2007

J. High Energy Phys.

151

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“…In figure 8, we show the posterior probability distribution for the rate of neutrino induced muons from dark matter annihilations in the Sun in a experiment such as SuperKamiokande (left) [60] and in a kilometer-scale, high energy neutrino telescope such as IceCube (right) [61]. For Super-Kamiokande, we plot the rate of muons with an energy…”

Section: Jhep10(2008)071mentioning

confidence: 99%

“…Currently, the strongest constraint on the neutrino flux from dark matter annihilations in the Sun comes from Super-Kamiokande, which has placed an upper limit on the rate of neutrino-induced muons from the Sun of approximately 3 × 10 3 per square kilometer, per year [60]. Slightly weaker constraints have also been placed by Amanda [62], Baksan [63] and Macro [64].…”

Section: Jhep10(2008)071mentioning

confidence: 99%

Panglossian prospects for detecting neutralino dark matter in light of natural priors?

Allanach

2008

J. High Energy Phys.

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In most global fits of the constrained minimal supersymmetric model (CMSSM) to indirect data, the a priori likelihoods of any two points in tan β are treated as equal, and the more fundamental µ and B Higgs potential parameters are fixed by potential minimization conditions. We find that, if instead a flat ("natural") prior measure on µ and B is placed, a strong preference exists for the focus point region from fits to particle physics and cosmological data. In particular, we find that the lightest neutralino is strongly favored to be a mixed bino-higgsino (∼ 10% higgsino). Such mixed neutralinos have large elastic scattering cross sections with nuclei, leading to extremely promising prospects for both underground direct detection experiments and neutrino telescopes. In particular, the majority of the posterior probability distribution falls within parameter space within an order of magnitude of current direct detection constraints. Furthermore, neutralino annihilations in the sun are predicted to generate thousands of neutrino induced muon events per years at IceCube. Thus, assuming the framework of the CMSSM and using the natural prior measure, modulo caveats regarding astrophysical uncertainties, we are likely to be living in a world with good prospects for the direct and indirect detection of neutralino dark matter.

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“…The SK experiment has taken data for 1679.6 days with an effective area of 10 3 m 2 , and set an upper limit on the number of high energy neutrinos above a GeV beyond the atmospheric neutrino background, which is around ∼ 10 [35,36]. We will consider the GDM mass above a few GeV scale.…”

mentioning

confidence: 99%

HiddenSU(N)glueball dark matter

2016

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We investigate the possibility that the dark matter candidate is from a pure non-abelian gauge theory of the hidden sector, motivated in large part by its elegance and simplicity. The dark matter is the lightest bound state made of the confined gauge fields, the hidden glueball. We point out this simple setup is capable of providing rich and novel phenomena in the dark sector, especially in the parameter space of large N . They include self-interacting and warm dark matter scenarios, Bose-Einstein condensation leading to massive dark stars possibly millions of times heavier than our sun giving rise to gravitational lensing effects, and indirect detections through higher dimensional operators as well as interesting collider signatures.

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Search for dark matter WIMPs using upward through-going muons in Super-Kamiokande

Cited by 269 publications

References 66 publications

Implications for the Constrained MSSM from a new prediction forb→sγ

Implications for the Constrained MSSM from a new prediction forb→sγ

Panglossian prospects for detecting neutralino dark matter in light of natural priors?

HiddenSU(N)glueball dark matter

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