Electron antineutrino search at the Sudbury Neutrino Observatory

Aharmim, B; Ahmed, S N; Beier, E W; Bellerive, A; Biller, S D; Boger, J; Boulay, M G; Bowles, T J; Brice, S J; Bullard, T V; Chan, Y D; Chen, M; Chen, X; Cleveland, B T; Cox, G A; Dai, X; Dalnoki-Veress, F; Doe, P J; Dosanjh, R S; Doucas, G; Dragowsky, M R; Duba, C A; Duncan, F A; Dunford, M; Dunmore, J A; Earle, E D; Elliott, S R; Evans, H C; Ewan, G T; Farine, J; Fergani, H; Fleurot, F; Formaggio, J A; Fowler, M M; Frame, K; Frati, W; Fulsom, B G; Gagnon, N; Graham, K; Grant, D R; Hahn, RL; Hallin, AL; Hallman, E D; Hamer, A S; Handler, W B; Hargrove, C K; Harvey, P J; Hazama, R; Heeger, K M; Heintzelman, W J; Heise, J; Helmer, R L; Hemingway, R J; Hime, A; Howe, M A; Jagam, P; Jelley, N A; Klein, J R; Kormos, L L; Kos, M S; Kruger, A; Krauss, C B; Krumins, A V; Kutter, T; Kyba, C C M; Labranche, H; Lange, R; Law, J; Lawson, I T; Lesko, K T; Leslie, J R; Levine, I; Luoma, S; MacLellan, R; Majerus, S; Mak, H B; Maneira, J; Marino, A D; McCauley, N; McDonald, A B; McGee, S; McGregor, G; Mifflin, C; Miknaitis, K K S; Miller, G G; Moffat, B A; Nally, C W; Neubauer, M S; Nickel, B G; Noble, A J; Norman, E B; Oblath, N S; Okada, C E; Ollerhead, R W; Orrell, J L; Oser, S M; Ouellet, C; Peeters, Simon; Poon, A W P; Rielage, K; Robertson, B C; Robertson, R G H; Rollin, E; Rosendahl, S S E; Rusu, V L; Schwendener, M H; Simard, O; Simpson, J J; Sims, C J; Sinclair, D; Skensved, P; Smith, M W E; Starinsky, N; Stokstad, RG; Stonehill, LC; Tafirout, R; Takeuchi, Y; Tesic, G; Thomson, M; Tsui, T; Van, B; Van de Water, R G; Virtue, C J; Wall, B L; Waller, D; Waltham, C E; Tseung, H W C; Wark, D L; West, N; Wilhelmy, J B; Wilkerson, J F; Wilson, J R; Wittich, P; Wouters, J M; Yeh, M; Zuber, K; SNO Collaboration,

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Electron antineutrino search at the Sudbury Neutrino Observatory

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posted on 2023-06-07, 22:21 authored by B Aharmim, S N Ahmed, E W Beier, A Bellerive, S D Biller, J Boger, M G Boulay, T J Bowles, S J Brice, T V Bullard, Y D Chan, M Chen, X Chen, B T Cleveland, G A Cox, X Dai, F Dalnoki-Veress, P J Doe, R S Dosanjh, G Doucas, M R Dragowsky, C A Duba, F A Duncan, M Dunford, J A Dunmore, E D Earle, S R Elliott, H C Evans, G T Ewan, J Farine, H Fergani, F Fleurot, J A Formaggio, M M Fowler, K Frame, W Frati, B G Fulsom, N Gagnon, K Graham, D R Grant, RL Hahn, AL Hallin, E D Hallman, A S Hamer, W B Handler, C K Hargrove, P J Harvey, R Hazama, K M Heeger, W J Heintzelman, J Heise, R L Helmer, R J Hemingway, A Hime, M A Howe, P Jagam, N A Jelley, J R Klein, L L Kormos, M S Kos, A Kruger, C B Krauss, A V Krumins, T Kutter, C C M Kyba, H Labranche, R Lange, J Law, I T Lawson, K T Lesko, J R Leslie, I Levine, S Luoma, R MacLellan, S Majerus, H B Mak, J Maneira, A D Marino, N McCauley, A B McDonald, S McGee, G McGregor, C Mifflin, K K S Miknaitis, G G Miller, B A Moffat, C W Nally, M S Neubauer, B G Nickel, A J Noble, E B Norman, N S Oblath, C E Okada, R W Ollerhead, J L Orrell, S M Oser, C Ouellet, Simon PeetersSimon Peeters, A W P Poon, K Rielage, B C Robertson, R G H Robertson, E Rollin, S S E Rosendahl, V L Rusu, M H Schwendener, O Simard, J J Simpson, C J Sims, D Sinclair, P Skensved, M W E Smith, N Starinsky, RG Stokstad, LC Stonehill, R Tafirout, Y Takeuchi, G Tesic, M Thomson, T Tsui, B Van, R G Van de Water, C J Virtue, B L Wall, D Waller, C E Waltham, H W C Tseung, D L Wark, N West, J B Wilhelmy, J F Wilkerson, J R Wilson, P Wittich, J M Wouters, M Yeh, K Zuber, SNO Collaboration

Upper limits on the (ν) over bar (e) flux at the Sudbury Neutrino Observatory have been set based on the (ν) over bar (e) 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 (ν) over bar (e)'s from the Sun and other potential sources. Both differential and integral limits on the (ν) over bar (e) flux have been placed in the energy range from 4-14.8 MeV. For an energy-independent nu(e)-->(ν) over bar (e) conversion mechanism, the integral limit on the flux of solar (ν) over bar (e)'s in the energy range from 4-14.8 MeV is found to be Phi(nue)less than or equal to3.4x10(4) cm(-2) s(-1) (90% C.L.), which corresponds to 0.81% of the standard solar model B-8 nu(e) flux of 5.05x10(6) cm(-2) s(-1), and is consistent with the more sensitive limit from KamLAND in the 8.3-14.8 MeV range of 3.7x10(2) cm(-2) s(-1) (90% C.L.). In the energy range from 4-8 MeV, a search for (ν) over bar (e)'s is conducted using coincidences in which only the two neutrons are detected. Assuming a (ν) over bar (e) spectrum for the neutron induced fission of naturally occurring elements, a flux limit of Phi((ν) over bare)less than or equal to2.0x10(6) cm(-2) s(-1) (90% C.L.) is obtained.

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Journal

Physical Review D

ISSN

0556-2821

External DOI

https://doi.org/10.1103/PhysRevD.70.093014

Issue

9

Volume

70

Page range

093014

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Physics and Astronomy Publications

Full text available

Yes

Peer reviewed?

Yes

Legacy Posted Date

2012-02-06

First Open Access (FOA) Date

2016-03-22

First Compliant Deposit (FCD) Date

2017-03-13

Electron antineutrino search at the Sudbury Neutrino Observatory

History

Publication status

File Version

Journal

ISSN

External DOI

Issue

Volume

Page range

Department affiliated with

Full text available

Peer reviewed?

Legacy Posted Date

First Open Access (FOA) Date

First Compliant Deposit (FCD) Date

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