Independent Measurement of the Total Active<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">B</mml:mi><mml:mprescripts /><mml:none /><mml:mn>8</mml:mn></mml:mmultiscripts></mml:math>Solar Neutrino Flux Using an Array of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi>He</mml:mi><mml:mprescripts /><mml:none /><mml:mn>3</mml:mn></mml:mmultiscripts></mml:math>Proportional Counters at th

Aharmim, B.; Ahmed, S.; Amsbaugh, J. F.; Anthony, A. E.; Banar, J.; Barros, N.; Beier, E. W.; Bellerive, A.; Beltrán, B.; Bergevin, M.; Biller, S. D.; Boudjemline, K.; Boulay, M. G.; Bowles, T. J.; Browne, M. C.; Bullard, T. V.; Burritt, T. H.; Cai, B.; Chan, Y. D.; Chauhan, D.; Chen, M.; Cleveland, B. T.; Cox-Mobrand, G. A.; Currat, C.; Dai, Xiongxin; Deng, Hui; Detwiler, J. A.; DiMarco, M.; Doe, P. J.; Doucas, G.; Drouin, P.‐L.; Duba, C. A.; Duncan, F. A.; Dunford, M.; Earle, E.D.; Elliott, S. R.; Evans, H. C.; Ewan, G. T.; Farine, J.; Fergani, H.; Fleurot, F.; Ford, R.; Formaggio, J. A.; Fowler, Μ. M.; Gagnon, N.; Germani, J. V.; Goldschmidt, A.; Goon, J. Tm.; Graham, K.; Guillian, E.; Habib, S.; Hahn, R. L.; Hallin, A. L.; Hallman, E. D.; Hamian, A. A.; Harper, G.; Harvey, P. J.; Hazama, R.; Heeger, K. M.; Heintzelman, W. J.; Heise, J.; Helmer, R. L.; Henning, R.; Hime, A.; Howard, C.; Howe, M. A.; Huang, M.; Jagam, P.; Jamieson, B.; Jelley, N. A.; Keeter, K. J.; Klein, J.; Kormos, L. L.; Kos, M.; Krüger, A.; Kraus, C.; Krauss, C. B.; Kutter, T.; Kyba, Christopher C. M.; Lange, R.; Law, J.; Lawson, I.; Lesko, K. T.; Leslie, J. R.; Loach, J. C.; MacLellan, R.; Majerus, Steve; Mak, H. B.; Maneira, J.; Martin, R. D.; McBryde, Kevin; McCauley, N.; McDonald, A.B.; McGee, Steven; Mifflin, C.; Miller, Guthrie; Miller, Michael L.; Monreal, B.; Monroe, J.; Morissette, B.; Myers, A.W.; Nickel, B. G.; Noble, A. J.; Oblath, N. S.; O’Keeffe, H. M.; Ollerhead, R. W.; Gann, G. D. Orebi; Oser, S. M.; Ott, R. A.; Peeters, S. J. M.; Poon, A. W. P.; Prior, G.; Reitzner, S. D.; Rielage, K.; Robertson, B.C.; Robertson, R. G. H.; Rollin, E.; Schwendener, M. H.; Secrest, J. A.; Seibert, S.; Simard, O.; Simpson, John; Sinclair, L.E.; Skensved, P.; Smith, M. W. E.; Steiger, Thomas; Stonehill, L. C.; Tešić, G.; Thornewell, P. M.; Tolich, N.; Tsui, T.; Tunnell, C.; Wechel, T. Van; Berg, R. Van; VanDevender, B. A.; Virtue, C. J.; Walker, Thomas J.; Wall, B. L.; Waller, D.; Tseung, H. Wan Chan; Wendland, J.; West, N.; Wilhelmy, J.B.; Wilkerson, J. F.; Wilson, J. R.; Wouters, J.M.; Wright, A.; Yeh, M.; Zhang, F.; Zuber, Κ.

doi:10.1103/physrevlett.101.111301

Cited by 286 publications

(189 citation statements)

References 29 publications

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“…For real-time experiments we include the 44 data points of the electron scattering (ES) Super-Kamiokande phase I (SK-I) energy-zenith spectrum [17] and the data from the three phases of SNO [18][19][20], including the results on the low energy threshold analysis of the combined SNO phase I and phase II [21] (which we label SNO-LETA). We also include the main set of the 192 days of Borexino data [22] (which we label Borexino-LE) as well as their high-energy spectrum from 246 live days [23] (Borexino-HE).…”

Section: Leading ∆M 2 21 Oscillations: Solar and Kamland Datamentioning

confidence: 99%

Updated global fit to three neutrino mixing: status of the hints of θ 13 > 0

Gonzalez-Garcia

Maltoni

Salvadó

2010

J. High Energ. Phys.

241

145

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Abstract:We present an up-to-date global analysis of solar, atmospheric, reactor and accelerator neutrino data in the framework of three-neutrino oscillations. We discuss in detail the statistical significance of the observed "hint" of non-zero θ 13 in the solar sector at the light of the latest experimental advances, such as the Borexino spectral data, the lower value of Gallium rate recently measured in SAGE, and the low energy threshold analysis of the combined SNO phase I and phase II. We also study the robustness of the results under changes of the inputs such as the choice of solar model fluxes and a possible modification of the Gallium capture cross-section as proposed by SAGE. In the atmospheric sector we focus on the latest results for ν e appearance from MINOS and on the recent SuperKamiokande results from the combined phases I, II and III, and we discuss their impact on the determination of θ 13 . Finally, we combine all the data into a global analysis and determine the presently allowed ranges of masses and mixing.

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Section: Leading ∆M 2 21 Oscillations: Solar and Kamland Datamentioning

confidence: 99%

Updated global fit to three neutrino mixing: status of the hints of θ 13 > 0

Gonzalez-Garcia

Maltoni

Salvadó

2010

J. High Energ. Phys.

241

145

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show abstract

“…By exploiting particle identification information obtained from the proportional counters installed during the third phase, this analysis improved background rejection in that phase of the experiment. The combined analysis resulted in a total flux of active neutrino flavors from 8 B decays in the Sun of (5.25 ± 0.16(stat. )…”

mentioning

confidence: 99%

Combined analysis of all three phases of solar neutrino data from the Sudbury Neutrino Observatory

et al. 2013

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“…A two-neutrino oscillation analysis [51] Thus far, we have seen that ν µ s disappear via ∆m 2 atm -driven oscillations, presum- 13 The comparison is actually more subtle, as we will soon see.…”

mentioning

confidence: 92%

Electron Neutrino Appearance in the MINOS Experiment

Orchanian

2012

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Independent Measurement of the Total ActiveB8Solar Neutrino Flux Using an Array ofHe3Proportional Counters at th

Cited by 286 publications

References 29 publications

Updated global fit to three neutrino mixing: status of the hints of θ 13 > 0

Updated global fit to three neutrino mixing: status of the hints of θ 13 > 0

Combined analysis of all three phases of solar neutrino data from the Sudbury Neutrino Observatory

Electron Neutrino Appearance in the MINOS Experiment

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