Evidence for Oscillation of Atmospheric Neutrinos

Fukuda, Y.; Hayakawa, Tomokatsu; Ichihara, E.; Inoue, K.; Ishihara, K.; Ishino, H.; Itow, Y.; Kajita, T.; Kameda, J.; Kasuga, S.; Kobayashi, Kazuyoshi; Kobayashi, Yoshiyuki; Koshio, Y.; Miura, M.; Nakahata, M.; Nakayama, S.; Okada, Atsushi; Okumura, K.; Sakurai, N.; Shiozawa, M.; Suzuki, Y.; Takeuchi, Y.; Totsuka, Y.; Yamada, Shoichi; Earl, M.; Habig, A.; Kearns, E.; Messier, M. D.; Scholberg, K.; Stone, J. L.; Sulak, L.; Walter, C. W.; Goldhaber, M.; Barszczxak, T.; Casper, D.; Gajewski, W.; Halverson, P. G.; Hsu, Jonathan Y.; Kropp, W. R.; Price, L. R.; Reines, F.; Smy, M. B.; Sobel, H. W.; Vagins, M. R.; Ganezer, K. S.; Keig, W. E.; Ellsworth, R. W.; Tasaka, S.; Flanagan, J.; Kibayashi, A.; Learned, J. G.; Matsuno, S.; Stenger, V. J.; Takemori, D.; Ishii, T.; Kanzaki, J.; Kobayashi, T.; Mine, S.; Nakamura, K.; Nishikawa, K.; Oyama, Y.; Sakai, Akito; Sakuda, M.; Sasaki, O.; Echigo, S.; Kohama, M.; Suzuki, A.; Haines, T. J.; Blaufuss, E.; Kim, B. K.; Sanford, R.; Svoboda, R.; Chen, M. L.; Conner, Z.; Goodman, J. A.; Sullivan, G. W.; Hill, J.; Jung, C. K.; Martens, K.; Mauger, C.; McGrew, C.; Sharkey, E.; Viren, B.; Yanagisawa, C.; Doki, W.; Miyano, K.; Okazawa, H.; Saji, C.; Takahata, M.; Nagashima, Y.; Takita, M.; Yamaguchi, Tomohiro; Yoshida, Masato; Kim, S. B.; Etoh, M.; Fujita, K.; Hasegawa, T.; Hasegawa, T.; Hatakeyama, S.; Iwamoto, Toshiyuki; Koga, M.; Maruyama, T.; Ogawa, Hiroshi; Shirai, J.; Tsushima, F.; Koshiba, M.; Nemoto, Mariko; Nishijima, K.; Futagami, T.; Hayato, Y.; Kanaya, Yoshio; Kaneyuki, K.; Watanabe, Y.; Kiełczewska, D.; Doyle, R. A.; George, Jimin; Stachyra, A. L.; Wai, L.; Wilkes, R. J.; Young, K. K.

doi:10.1103/physrevlett.81.1562

Cited by 4,440 publications

(2,969 citation statements)

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“…Atmospheric neutrinos oscillate with a large mixing angle [38] and all the currently allowed solar oscillations correspond to large mixing angles (see figure 1).…”

Section: Allowed Ranges Of Mass Mixing Angle and 8 B Neutrino Fluxmentioning

confidence: 99%

Before and After: How has the SNO NC measurement changed things?

Bahcall¹,

González-García²,

Peña-Garay³

2002

J. High Energy Phys.

126

121

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We present "Before and After" global oscillation solutions, as well as predicted "Before and After" values and ranges for ten future solar neutrino observables (for BOREXINO, KamLAND, SNO, and a generic p − p neutrino detector). The "Before" case includes all solar neutrino data (and some theoretical improvements) available prior to April 20, 2002 and the "After" case includes, in addition, the new SNO data on the CC, NC, and day-night asymmetry. We have performed global analyses using the full SNO day-night energy spectrum and, alternatively, using just the SNO NC and CC rates and the day-night asymmetry. The LMA solution is the only currently allowed MSW oscillation solution at ∼ 99% CL. The LOW solution is allowed only at more than 2.5σ, SMA is now excluded at 3.7σ or 4.7σ depending upon analysis strategy, and pure sterile oscillations are excluded at more than 4.7σ. Small mixing angles are "out" (pure sterile is "way out"); MSW with large mixing angles is definitely "in." Vacuum oscillations are allowed at 3σ, but not at 2σ. Precise maximal mixing is excluded at 3.2σ for MSW solutions and at more than 2.8σ for vacuum solutions. Most of the predicted values for future observables for the BOREXINO, KamLAND, and future SNO measurements are changed only by minor amounts by the inclusion of the recent SNO data. In order to test the robustness of the allowed neutrino oscillation regions that are inferred from the measurements and the predicted values for future solar neutrino observables, we have carried out calculations using a variety of strategies for analyzing the SNO and other experimental data.

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“…Atmospheric neutrinos oscillate with a large mixing angle [38] and all the currently allowed solar oscillations correspond to large mixing angles (see figure 1).…”

Section: Allowed Ranges Of Mass Mixing Angle and 8 B Neutrino Fluxmentioning

confidence: 99%

Before and After: How has the SNO NC measurement changed things?

Bahcall¹,

González-García²,

Peña-Garay³

2002

J. High Energy Phys.

126

121

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“…energy-scale calibration factor, whose small uncertainty (1.1%) is practically negligible: 8) where N C = 14 is the number of energy bins and α C is the absolute normalization constant with uncertainty σ α C = 2.7 × 10 −2 [33]. We calculate the CHOOZ covariance matrix V C as described in Eq.…”

Section: Rates Analysismentioning

confidence: 99%

“…[6] for a discussion on the probability content of this statement). Since the simplest explanation of the presence of ν µ or ν τ in the flux of solar neutrino on Earth is neutrino oscillations due to neutrino masses and mixing (see [7]), this is the second model-independent evidence in favor of neutrino mixing, after the up-down asymmetry of multi-GeV atmospheric ν µ -induced events discovered in the Super-Kamiokande experiment [8].…”

Section: Introductionmentioning

confidence: 99%

Bayesian view of solar neutrino oscillations

Garzelli

Giunti

2001

J. High Energy Phys.

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We present the results of a Bayesian analysis of solar neutrino data in terms of ν e → ν µ,τ and ν e → ν s oscillations, where ν s is a sterile neutrino. We perform a Rates Analysis of the rates of solar neutrino experiments, including the first SNO CC result, and spectral data of the CHOOZ experiment, and a Global Analysis that takes into account also the Super-Kamiokande day and night electron energy spectra. We show that the Bayesian analysis of solar neutrino data does not suffer any problem from the inclusion of the numerous bins of the CHOOZ and Super-Kamiokande electron energy spectra and allows to reach the same conclusions on the favored type of neutrino transitions and on the determination of the most favored values of the oscillation parameters in both the Rates and Global Analysis. Our Bayesian analysis shows that ν e → ν s transitions are strongly disfavored with respect to ν e → ν µ,τ transitions. In the case of ν e → ν µ,τ oscillations, the Large Mixing Angle region is favored by the data (86% probability), the LOW region has some small chance (13% probability), the Vacuum Oscillation region is almost excluded (1% probability) and the Small Mixing Angle region is practically excluded (0.01% probability). We calculate also the marginal posterior probability distributions for tan 2 ϑ and ∆m 2 in the case of ν e → ν µ,τ oscillations and we show that the data imply large mixing almost with certainty and large values of ∆m 2 are favored (2 × 10 −6 eV 2 < ∆m 2 < 10 −3 eV 2 with 86% probability). We present also the results of a standard least-squares analysis of solar neutrino data and we show that the standard goodness of fit test is not able to reject pure ν e → ν s transitions. The likelihood ratio test, which is insensitive to the number of bins of the CHOOZ and Super-Kamiokande energy spectra, allows to reject pure ν e → ν s transitions in favor of ν e → ν µ,τ transitions only in the Global Analysis.

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“…The experimental confirmation that atmospheric and solar neutrinos do oscillate [1,2], and therefore have mass, represents the first solid clue for the existence of new physics beyond the Standard Model [3]. Results from experiments carried out with neutrinos produced in artificial sources, like reactors and accelerators, strongly support the fact that neutrinos are massive [4,5].…”

Section: Introductionmentioning

confidence: 99%