Electron antineutrino search at the Sudbury Neutrino Observatory

Authors

B. Aharmim, Laurentian University
S. N. Ahmed, Queen’s University
E. W. Beier, University of Pennsylvania
A. Bellerive, Carleton University
S. D. Biller, University of Oxford
J. Boger, Brookhaven National Laboratory
M. G. Boulay, Los Alamos National Laboratory
T. J. Bowles, Los Alamos National Laboratory
S. J. Brice, Los Alamos National Laboratory
T. V. Bullard, University of Washington
Y. D. Chan, Lawrence Berkeley National Laboratory
M. Chen, Queen’s University
X. Chen, Lawrence Berkeley National Laboratory
B. T. Cleveland, University of Oxford
G. A. Cox, University of Washington
X. Dai, Carleton University
F. Dalnoki-Veress, Carleton University
P. J. Doe, University of Washington
R. S. Dosanjh, Carleton University
G. Doucas, University of Oxford
M. R. Dragowsky, Los Alamos National Laboratory
C. A. Duba, University of Washington
F. A. Duncan, Queen’s University
M. Dunford, University of Pennsylvania
J. A. Dunmore, University of Oxford
E. D. Earle, Queen’s University
S. R. Elliott, Los Alamos National Laboratory
H. C. Evans, Queen’s University

Document Type

Article

Publication Date

1-1-2004

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]’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. © 2004 The American Physical Society.

Publication Source (Journal or Book title)

Physical Review D - Particles, Fields, Gravitation and Cosmology

Recommended Citation

Aharmim, B., Ahmed, S., Beier, E., Bellerive, A., Biller, S., Boger, J., Boulay, M., Bowles, T., Brice, S., Bullard, T., Chan, Y., Chen, M., Chen, X., Cleveland, B., Cox, G., Dai, X., Dalnoki-Veress, F., Doe, P., Dosanjh, R., Doucas, G., Dragowsky, M., Duba, C., Duncan, F., Dunford, M., Dunmore, J., Earle, E., Elliott, S., & Evans, H. (2004). Electron antineutrino search at the Sudbury Neutrino Observatory. Physical Review D - Particles, Fields, Gravitation and Cosmology, 70 (9) https://doi.org/10.1103/PhysRevD.70.093014