Determination of the _e and total ⁸B solar neutrino fluxes using the Sudbury Neutrino Observatory Phase I data set

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B. Aharmim,⁷ Q. R. Ahmad,²² S. N. Ahmed,¹⁷ R. C. Allen,⁴ T. C. Andersen,⁶ J. D. Anglin,¹³ G. Bühler,⁴ J. C. Barton,¹⁴ E. W. Beier,¹⁵ M. Bercovitch,¹³ M. Bergevin,^6,8 J. Bigu,⁷ S. D. Biller,¹⁴ R. A. Black,¹⁴ I. Blevis,⁵ R. J. Boardman,¹⁴ J. Boger,³ E. Bonvin,¹⁷ M. G. Boulay,^10,17 M. G. Bowler,¹⁴ T. J. Bowles,¹⁰ S. J. Brice,^10,14 M. C. Browne,^10,22 T. V. Bullard,²² T. H. Burritt,²² J. Cameron,¹⁴ Y. D. Chan,⁸ H. H. Chen,⁴ M. Chen,¹⁷ X. Chen,⁸ B. T. Cleveland,¹⁴ J. H. M. Cowan,⁷ D. F. Cowen,¹⁵ G. A. Cox,²² C. A. Currat,⁸ X. Dai,^5,14,17 F. Dalnoki-Veress,⁵ W. F. Davidson,¹³ H. Deng,¹⁵ M. DiMarco,¹⁷ P. J. Doe,²² G. Doucas,¹⁴ M. R. Dragowsky,^8,10 C. A. Duba,²² F. A. Duncan,^17,19 M. Dunford,¹⁵ J. A. Dunmore,¹⁴ E. D. Earle,¹⁷ S. R. Elliott,^10,22 H. C. Evans,¹⁷ G. T. Ewan,¹⁷ J. Farine,⁷ H. Fergani,¹⁴ A. P. Ferraris,¹⁴ F. Fleurot,⁷ R. J. Ford,^17,19 J. A. Formaggio,¹² M. M. Fowler,¹⁰ K. Frame,^5,14 E. D. Frank,¹⁵ W. Frati,¹⁵ N. Gagnon,^8,10,14,22 J. V. Germani,^10,22 S. Gil,² A. Goldschmidt,¹⁰ J. T. M. Goon,¹¹ K. Graham,⁵ D. R. Grant,⁵ E. Guillian,¹⁷ R. L. Hahn,³ A. L. Hallin,¹⁷ E. D. Hallman,⁷ A. S. Hamer,^10,17 A. A. Hamian,²² W. B. Handler,¹⁷ R. U. Haq,⁷ C. K. Hargrove,⁵ P. J. Harvey,¹⁷ R. Hazama,²² K. M. Heeger,²² W. J. Heintzelman,¹⁵ J. Heise,^2,10,17 R. L. Helmer,²¹ R. Henning,⁸ J. D. Hepburn,¹⁷ H. Heron,¹⁴ J. Hewett,⁷ A. Hime,¹⁰ C. Howard,¹⁷ M. A. Howe,²² M. Huang,²⁰ J. G. Hykaway,⁷ M. C. P. Isaac,⁸ P. Jagam,⁶ B. Jamieson,² N. A. Jelley,¹⁴ C. Jillings,¹⁷ G. Jonkmans,^1,7 K. Kazkaz,²² P. T. Keener,¹⁵ K. Kirch,¹⁰ J. R. Klein,²⁰ A. B. Knox,¹⁴ R. J. Komar,² L. L. Kormos,¹⁷ M. Kos,¹⁷ R. Kouzes,¹⁶ A. Krüger,⁷ C. Kraus,¹⁷ C. B. Krauss,¹⁷ T. Kutter,¹¹ C. C. M. Kyba,¹⁵ H. Labranche,⁶ R. Lange,³ J. Law,⁶ I. T. Lawson,^6,19 M. Lay,¹⁴ H. W. Lee,¹⁷ K. T. Lesko,⁸ J. R. Leslie,¹⁷ I. Levine,⁵ J. C. Loach,¹⁴ W. Locke,¹⁴ S. Luoma,⁷ J. Lyon,¹⁴ R. MacLellan,¹⁷ S. Majerus,¹⁴ H. B. Mak,¹⁷ J. Maneira,⁹ A. D. Marino,⁸ R. Martin,¹⁷ N. McCauley,^14,15 A. B. McDonald,¹⁷ D. S. McDonald,¹⁵ K. McFarlane,⁵ S. McGee,²² G. McGregor,¹⁴ R. Meijer Drees,²² H. Mes,⁵ C. Mifflin,⁵ K. K. S. Miknaitis,²² M. L. Miller,¹² G. Milton,¹ B. A. Moffat,¹⁷ B. Monreal,¹² M. Moorhead,^8,14 B. Morrissette,¹⁹ C. W. Nally,² M. S. Neubauer,¹⁵ F. M. Newcomer,¹⁵ H. S. Ng,² B. G. Nickel,⁶ A. J. Noble,¹⁷ E. B. Norman,⁸ V. M. Novikov,⁵ N. S. Oblath,²² C. E. Okada,⁸ H. M. O'Keeffe,¹⁴ R. W. Ollerhead,⁶ M. Omori,¹⁴ J. L. Orrell,²² S. M. Oser,² R. Ott,¹² S. J. M. Peeters,¹⁴ A. W. P. Poon,⁸ G. Prior,⁸ S. D. Reitzner,⁶ K. Rielage,^10,22 A. Roberge,⁷ B. C. Robertson,¹⁷ R. G. H. Robertson,²² S. S. E. Rosendahl,⁸ J. K. Rowley,³ V. L. Rusu,¹⁵ E. Saettler,⁷ A. Schülke,⁸ M. H. Schwendener,⁷ J. A. Secrest,¹⁵ H. Seifert,^7,10,22 M. Shatkay,⁵ J. J. Simpson,⁶ C. J. Sims,¹⁴ D. Sinclair,^5,21 P. Skensved,¹⁷ A. R. Smith,⁸ M. W. E. Smith,^10,22 N. Starinsky,^5,8,10,22 T. D. Steiger,²² R. G. Stokstad,⁸ L. C. Stonehill,^10,22 R. S. Storey,¹³ B. Sur,^1,17 R. Tafirout,⁷ N. Tagg,^6,14 Y. Takeuchi,¹⁷ N. W. Tanner,¹⁴ R. K. Taplin,¹⁴ M. Thorman,¹⁴ P. M. Thornewell,^10,14,22 N. Tolich,⁸ P. T. Trent,¹⁴ Y. I. Tserkovnyak,² T. Tsui,² C. D. Tunnell,²⁰ R. Van Berg,¹⁵ R. G. Van de Water,^10,15 C. J. Virtue,⁷ T. J. Walker,¹² B. L. Wall,²² C. E. Waltham,² H. Wan Chan Tseung,¹⁴ J.-X. Wang,⁶ D. L. Wark,¹⁸ J. Wendland,² N. West,¹⁴ J. B. Wilhelmy,¹⁰ J. F. Wilkerson,²² J. R. Wilson,¹⁴ P. Wittich,¹⁵ J. M. Wouters,¹⁰ A. Wright,¹⁷ M. Yeh,³ and K. Zuber¹⁴

(SNO Collaboration)

¹Atomic Energy of Canada, Limited, Chalk River Laboratories, Chalk River, Ontario K0J 1J0, Canada
²Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia V6T 1Z1, Canada
³Chemistry Department, Brookhaven National Laboratory, Upton, New York 11973-5000, USA
⁴Department of Physics, University of California, Irvine, California 92717, USA
⁵Ottawa-Carleton Institute for Physics, Department of Physics, Carleton University, Ottawa, Ontario K1S 5B6, Canada
⁶Physics Department, University of Guelph, Guelph, Ontario N1G 2W1, Canada
⁷Department of Physics and Astronomy, Laurentian University, Sudbury, Ontario P3E 2C6, Canada
⁸Institute for Nuclear and Particle Astrophysics and Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
⁹Laboratório de Instrumentação e Física Experimental de Partículas, Av. Elias Garcia 14, 1^°, P-1000-149 Lisboa, Portugal
¹⁰Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
¹¹Department of Physics and Astronomy, Louisiana State University, Baton Rouge, Louisiana 70803, USA
¹²Laboratory for Nuclear Science, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA
¹³National Research Council of Canada, Ottawa, Ontario K1A 0R6, Canada
¹⁴Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, United Kingdom
¹⁵Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, Pennsylvania 19104-6396, USA
¹⁶Department of Physics, Princeton University, Princeton, New Jersey 08544, USA
¹⁷Department of Physics, Queen's University, Kingston, Ontario K7L 3N6, Canada
¹⁸Rutherford Appleton Laboratory, Chilton, Didcot OX11 0QX, United Kingdom
¹⁹SNOLAB, Sudbury, Ontario P3Y 1M3, Canada
²⁰Department of Physics, University of Texas at Austin, Austin, Texas 78712-0264, USA
²¹TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
²²Center for Experimental Nuclear Physics and Astrophysics, and Department of Physics, University of Washington, Seattle, Washington 98195, USA

Received 13 October 2006; published 27 April 2007

Thisarticle provides the complete description of results from the PhaseI data set of the Sudbury Neutrino Observatory (SNO). ThePhase I data set is based on a 0.65 kiloton-yearexposure of ²H₂O (in the following denoted as D₂O) tothe solar ⁸B neutrino flux. Included here are details ofthe SNO physics and detector model, evaluations of systematic uncertainties,and estimates of backgrounds. Also discussed are SNO's approach tostatistical extraction of the signals from the three neutrino reactions(charged current, neutral current, and elastic scattering) and the resultsof a search for a day-night asymmetry in the _eflux. Under the assumption that the ⁸B spectrum is undistorted,the measurements from this phase yield a solar _e fluxof phi (_e)=1.76 -0.05+0.05 (stat.) -0.09+0.09 (syst.)×10⁶ cm^-2 s^-1 and a non-_e component of phi (_µ)=3.41 -0.45+0.45 (stat.) -0.45+0.48 (syst.)×10⁶cm^-2 s^-1. The sum of these components provides a totalflux in excellent agreement with the predictions of standard solarmodels. The day-night asymmetry in the _e flux is foundto be A_e=7.0±4.9(stat.) -1.2+1.3 %(syst.), when the asymmetry in the total fluxis constrained to be zero.

URL:	http://link.aps.org/doi/10.1103/PhysRevC.75.045502
DOI:	10.1103/PhysRevC.75.045502
PACS:	26.65.+t; 14.60.Pq; 13.15.+g; 95.85.Ry 26.65.+t Solar neutrinos in nuclear astrophysics 14.60.Pq Neutrino mass and mixing 13.15.+g Neutrino interactions 95.85.Ry Neutrino, muon, pion, and other elementary particle astronomical observations; cosmic rays YEAR: 2007

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Phys. Rev. C 75, 045502 (2007) [69 pages]

Determination of the e and total 8B solar neutrino fluxes using the Sudbury Neutrino Observatory Phase I data set

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Determination of the _e and total ⁸B solar neutrino fluxes using the Sudbury Neutrino Observatory Phase I data set