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Electron antineutrino search at the Sudbury Neutrino Observatory

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Electron antineutrino search at the Sudbury Neutrino Observatory. / SNO Collaboration ; Kormos, Laura.
In: Physical Review D - Particles, Fields, Gravitation and Cosmology, Vol. 70, No. 9, 093014, 01.01.2004.

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Harvard

SNO Collaboration & Kormos, L 2004, 'Electron antineutrino search at the Sudbury Neutrino Observatory', Physical Review D - Particles, Fields, Gravitation and Cosmology, vol. 70, no. 9, 093014. https://doi.org/10.1103/PhysRevD.70.093014

APA

SNO Collaboration, & Kormos, L. (2004). Electron antineutrino search at the Sudbury Neutrino Observatory. Physical Review D - Particles, Fields, Gravitation and Cosmology, 70(9), Article 093014. https://doi.org/10.1103/PhysRevD.70.093014

Vancouver

SNO Collaboration, Kormos L. Electron antineutrino search at the Sudbury Neutrino Observatory. Physical Review D - Particles, Fields, Gravitation and Cosmology. 2004 Jan 1;70(9):093014. doi: 10.1103/PhysRevD.70.093014

Author

SNO Collaboration ; Kormos, Laura. / Electron antineutrino search at the Sudbury Neutrino Observatory. In: Physical Review D - Particles, Fields, Gravitation and Cosmology. 2004 ; Vol. 70, No. 9.

Bibtex

@article{5cd67ce0767847b28bab465a2a6ca984,
title = "Electron antineutrino search at the Sudbury Neutrino Observatory",
abstract = "Upper limits on the [Formula Presented] flux at the Sudbury Neutrino Observatory have been set based on the [Formula Presented] charged-current reaction on deuterium. The reaction produces a positron and two neutrons in coincidence. This distinctive signature allows a search with very low background for [Formula Presented]{\textquoteright}s from the Sun and other potential sources. Both differential and integral limits on the [Formula Presented] flux have been placed in the energy range from 4–14.8 MeV. For an energy-independent [Formula Presented] conversion mechanism, the integral limit on the flux of solar [Formula Presented]{\textquoteright}s in the energy range from 4–14.8 MeV is found to be [Formula Presented] (90% C.L.), which corresponds to 0.81% of the standard solar model [Formula presented] [Formula Presented] flux of [Formula Presented], and is consistent with the more sensitive limit from KamLAND in the 8.3–14.8 MeV range of [Formula Presented] (90% C.L.). In the energy range from 4–8 MeV, a search for [Formula Presented]{\textquoteright}s is conducted using coincidences in which only the two neutrons are detected. Assuming a [Formula Presented] spectrum for the neutron induced fission of naturally occurring elements, a flux limit of [Formula Presented] (90% C.L.) is obtained.",
author = "{SNO Collaboration} and B. Aharmim and Beier, {E. W.} and A. Bellerive and Biller, {S. D.} and J. Boger and Boulay, {M. G.} and Bowles, {T. J.} and Brice, {S. J.} and Bullard, {T. V.} and Cleveland, {B. T.} and X. Dai and F. Dalnoki-Veress and Doe, {P. J.} and Dosanjh, {R. S.} and G. Doucas and Dragowsky, {M. R.} and Duba, {C. A.} and Duncan, {F. A.} and M. Dunford and Dunmore, {J. A.} and Earle, {E. D.} and Evans, {H. C.} and Ewan, {G. T.} and J. Farine and H. Fergani and F. Fleurot and Formaggio, {J. A.} and Fowler, {M. M.} and K. Frame and W. Frati and Fulsom, {B. G.} and N. Gagnon and K. Graham and Grant, {D. R.} and Hahn, {R. L.} and Hallin, {A. L.} and Hallman, {E. D.} and Hamer, {A. S.} and Handler, {W. B.} and Hargrove, {C. K.} and Harvey, {P. J.} and R. Hazama and Heeger, {K. M.} and Heintzelman, {W. J.} and J. Heise and Helmer, {R. L.} and Hemingway, {R. J.} and A. Hime and P. Jagam and Jelley, {N. A.} and Laura Kormos",
year = "2004",
month = jan,
day = "1",
doi = "10.1103/PhysRevD.70.093014",
language = "English",
volume = "70",
journal = "Physical Review D - Particles, Fields, Gravitation and Cosmology",
issn = "1550-7998",
publisher = "American Physical Society",
number = "9",

}

RIS

TY - JOUR

T1 - Electron antineutrino search at the Sudbury Neutrino Observatory

AU - SNO Collaboration

AU - Aharmim, B.

AU - Beier, E. W.

AU - Bellerive, A.

AU - Biller, S. D.

AU - Boger, J.

AU - Boulay, M. G.

AU - Bowles, T. J.

AU - Brice, S. J.

AU - Bullard, T. V.

AU - Cleveland, B. T.

AU - Dai, X.

AU - Dalnoki-Veress, F.

AU - Doe, P. J.

AU - Dosanjh, R. S.

AU - Doucas, G.

AU - Dragowsky, M. R.

AU - Duba, C. A.

AU - Duncan, F. A.

AU - Dunford, M.

AU - Dunmore, J. A.

AU - Earle, E. D.

AU - Evans, H. C.

AU - Ewan, G. T.

AU - Farine, J.

AU - Fergani, H.

AU - Fleurot, F.

AU - Formaggio, J. A.

AU - Fowler, M. M.

AU - Frame, K.

AU - Frati, W.

AU - Fulsom, B. G.

AU - Gagnon, N.

AU - Graham, K.

AU - Grant, D. R.

AU - Hahn, R. L.

AU - Hallin, A. L.

AU - Hallman, E. D.

AU - Hamer, A. S.

AU - Handler, W. B.

AU - Hargrove, C. K.

AU - Harvey, P. J.

AU - Hazama, R.

AU - Heeger, K. M.

AU - Heintzelman, W. J.

AU - Heise, J.

AU - Helmer, R. L.

AU - Hemingway, R. J.

AU - Hime, A.

AU - Jagam, P.

AU - Jelley, N. A.

AU - Kormos, Laura

PY - 2004/1/1

Y1 - 2004/1/1

N2 - Upper limits on the [Formula Presented] flux at the Sudbury Neutrino Observatory have been set based on the [Formula Presented] charged-current reaction on deuterium. The reaction produces a positron and two neutrons in coincidence. This distinctive signature allows a search with very low background for [Formula Presented]’s from the Sun and other potential sources. Both differential and integral limits on the [Formula Presented] flux have been placed in the energy range from 4–14.8 MeV. For an energy-independent [Formula Presented] conversion mechanism, the integral limit on the flux of solar [Formula Presented]’s in the energy range from 4–14.8 MeV is found to be [Formula Presented] (90% C.L.), which corresponds to 0.81% of the standard solar model [Formula presented] [Formula Presented] flux of [Formula Presented], and is consistent with the more sensitive limit from KamLAND in the 8.3–14.8 MeV range of [Formula Presented] (90% C.L.). In the energy range from 4–8 MeV, a search for [Formula Presented]’s is conducted using coincidences in which only the two neutrons are detected. Assuming a [Formula Presented] spectrum for the neutron induced fission of naturally occurring elements, a flux limit of [Formula Presented] (90% C.L.) is obtained.

AB - Upper limits on the [Formula Presented] flux at the Sudbury Neutrino Observatory have been set based on the [Formula Presented] charged-current reaction on deuterium. The reaction produces a positron and two neutrons in coincidence. This distinctive signature allows a search with very low background for [Formula Presented]’s from the Sun and other potential sources. Both differential and integral limits on the [Formula Presented] flux have been placed in the energy range from 4–14.8 MeV. For an energy-independent [Formula Presented] conversion mechanism, the integral limit on the flux of solar [Formula Presented]’s in the energy range from 4–14.8 MeV is found to be [Formula Presented] (90% C.L.), which corresponds to 0.81% of the standard solar model [Formula presented] [Formula Presented] flux of [Formula Presented], and is consistent with the more sensitive limit from KamLAND in the 8.3–14.8 MeV range of [Formula Presented] (90% C.L.). In the energy range from 4–8 MeV, a search for [Formula Presented]’s is conducted using coincidences in which only the two neutrons are detected. Assuming a [Formula Presented] spectrum for the neutron induced fission of naturally occurring elements, a flux limit of [Formula Presented] (90% C.L.) is obtained.

U2 - 10.1103/PhysRevD.70.093014

DO - 10.1103/PhysRevD.70.093014

M3 - Journal article

AN - SCOPUS:42749105454

VL - 70

JO - Physical Review D - Particles, Fields, Gravitation and Cosmology

JF - Physical Review D - Particles, Fields, Gravitation and Cosmology

SN - 1550-7998

IS - 9

M1 - 093014

ER -