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34 results on '"Cleveland, BT"'

1. Results from the Baksan Experiment on Sterile Transitions (BEST)

Author

Barinov, VV, Cleveland, BT, Danshin, SN, Ejiri, H, Elliott, SR, Frekers, D, Gavrin, VN, Gorbachev, VV, Gorbunov, DS, Haxton, WC, Ibragimova, TV, Kim, I, Kozlova, Yu P, Kravchuk, LV, Kuzminov, VV, Lubsandorzhiev, BK, Malyshkin, Yu M, Massarczyk, R, Matveev, VA, Mirmov, IN, Nico, JS, Petelin, AL, Robertson, RGH, Sinclair, D, Shikhin, AA, Tarasov, VA, Trubnikov, GV, Veretenkin, EP, Wilkerson, JF, and Zvir, AI

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, Mathematical Sciences, Engineering, General Physics, Mathematical sciences, Physical sciences
Abstract

The Baksan Experiment on Sterile Transitions (BEST) was designed to investigate the deficit of electron neutrinos ν_{e} observed in previous gallium-based radiochemical measurements with high-intensity neutrino sources, commonly referred to as the "gallium anomaly," which could be interpreted as evidence for oscillations between ν_{e} and sterile neutrino (ν_{s}) states. A 3.414-MCi ^{51}Cr ν_{e} source was placed at the center of two nested Ga volumes and measurements were made of the production of ^{71}Ge through the charged current reaction, ^{71}Ga(ν_{e},e^{-})^{71}Ge, at two average distances. The measured production rates for the inner and the outer targets, respectively, are [54.9_{-2.4}^{+2.5}(stat)±1.4(syst)] and [55.6_{-2.6}^{+2.7}(stat)±1.4(syst)] atoms of ^{71}Ge/d. The ratio (R) of the measured rate of ^{71}Ge production at each distance to the expected rate from the known cross section and experimental efficiencies are R_{in}=0.79±0.05 and R_{out}=0.77±0.05. The ratio of the outer to the inner result is 0.97±0.07, which is consistent with unity within uncertainty. The rates at each distance were found to be similar, but 20%-24% lower than expected, thus reaffirming the anomaly. These results are consistent with ν_{e}→ν_{s} oscillations with a relatively large Δm^{2} (>0.5  eV^{2}) and mixing sin^{2}2θ (≈0.4).

Published
2022

2. Search for hep solar neutrinos and the diffuse supernova neutrino background using all three phases of the Sudbury Neutrino Observatory

Author

Aharmim, B, Ahmed, SN, Anthony, AE, Barros, N, Beier, EW, Bellerive, A, Beltran, B, Bergevin, M, Biller, SD, Blucher, E, Bonventre, R, Boudjemline, K, Boulay, MG, Cai, B, Callaghan, EJ, Caravaca, J, Chan, YD, Chauhan, D, Chen, M, Cleveland, BT, Cox, GA, Dai, X, Deng, H, Descamps, FB, Detwiler, JA, Doe, PJ, Doucas, G, Drouin, PL, Dunford, M, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Fleurot, F, Ford, RJ, Formaggio, JA, Gagnon, N, Gilje, K, Goon, JTM, Graham, K, Guillian, E, Habib, S, Hahn, RL, Hallin, AL, Hallman, ED, Harvey, PJ, Hazama, R, Heintzelman, WJ, Heise, J, Helmer, RL, Hime, A, Howard, C, Huang, M, Jagam, P, Jamieson, B, Jelley, NA, Jerkins, M, Keeter, KJ, Klein, JR, Kormos, LL, Kos, M, Kraus, C, Krauss, CB, Krüger, A, Kutter, T, Kyba, CCM, Labe, K, Land, BJ, Lange, R, Latorre, A, Law, J, Lawson, IT, Lesko, KT, Leslie, JR, Levine, I, Loach, JC, Maclellan, R, Majerus, S, Mak, HB, Maneira, J, Martin, RD, Mastbaum, A, McCauley, N, McDonald, AB, McGee, SR, Miller, ML, Monreal, B, Monroe, J, Nickel, BG, Noble, AJ, O'Keeffe, HM, Oblath, NS, Okada, CE, Ollerhead, RW, Orebi Gann, GD, Oser, SM, Ott, RA, Peeters, SJM, and Poon, AWP

Subjects
hep-ex, nucl-ex
Abstract

A search has been performed for neutrinos from two sources, the hep reaction in the solar pp fusion chain and the νe component of the diffuse supernova neutrino background (DSNB), using the full dataset of the Sudbury Neutrino Observatory with a total exposure of 2.47 kton-years after fiducialization. The hep search is performed using both a single-bin counting analysis and a likelihood fit. We find a best-fit flux that is compatible with solar model predictions while remaining consistent with zero flux, and set a one-sided upper limit of φhep

Published
2020

3. Cosmogenic neutron production at the Sudbury Neutrino Observatory

Author

Aharmim, B, Ahmed, SN, Anthony, AE, Barros, N, Beier, EW, Bellerive, A, Beltran, B, Bergevin, M, Biller, SD, Bonventre, R, Boudjemline, K, Boulay, MG, Cai, B, Callaghan, EJ, Caravaca, J, Chan, YD, Chauhan, D, Chen, M, Cleveland, BT, Cox, GA, Curley, R, Dai, X, Deng, H, Descamps, FB, Detwiler, JA, Doe, PJ, Doucas, G, Drouin, PL, Dunford, M, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Fleurot, F, Ford, RJ, Formaggio, JA, Gagnon, N, Gilje, K, Goon, JTM, Graham, K, Guillian, E, Habib, S, Hahn, RL, Hallin, AL, Hallman, ED, Harvey, PJ, Hazama, R, Heintzelman, WJ, Heise, J, Helmer, RL, Hime, A, Howard, C, Huang, M, Jagam, P, Jamieson, B, Jelley, NA, Jerkins, M, Kéfélian, C, Keeter, KJ, Klein, JR, Kormos, LL, Kos, M, Krüger, A, Kraus, C, Krauss, CB, Kutter, T, Kyba, CCM, Land, BJ, Lange, R, Law, J, Lawson, IT, Lesko, KT, Leslie, JR, Levine, I, Loach, JC, MacLellan, R, Majerus, S, Mak, HB, Maneira, J, Martin, RD, Mastbaum, A, McCauley, N, McDonald, AB, McGee, SR, Miller, ML, Monreal, B, Monroe, J, Nickel, BG, Noble, AJ, O'Keeffe, HM, Oblath, NS, Okada, CE, Ollerhead, RW, Orebi Gann, GD, Oser, SM, Ott, RA, Peeters, SJM, Poon, AWP, and Prior, G

Subjects
hep-ex, nucl-ex
Abstract

Neutrons produced in nuclear interactions initiated by cosmic-ray muons present an irreducible background to many rare-event searches, even in detectors located deep underground. Models for the production of these neutrons have been tested against previous experimental data, but the extrapolation to deeper sites is not well understood. Here we report results from an analysis of cosmogenically produced neutrons at the Sudbury Neutrino Observatory. A specific set of observables are presented, which can be used to benchmark the validity of geant4 physics models. In addition, the cosmogenic neutron yield, in units of 10-4 cm2/(g·μ), is measured to be 7.28±0.09(stat)-1.12+1.59(syst) in pure heavy water and 7.30±0.07(stat)-1.02+1.40(syst) in NaCl-loaded heavy water. These results provide unique insights into this potential background source for experiments at SNOLAB.

Published
2019

4. Electromagnetic backgrounds and potassium-42 activity in the DEAP-3600 dark matter detector

Author

Ajaj, R, Araujo, GR, Batygov, M, Beltran, B, Bina, CE, Boulay, MG, Broerman, B, Bueno, JF, Burghardt, PM, Butcher, A, Cai, B, Cárdenas-Montes, M, Cavuoti, S, Chen, M, Chen, Y, Cleveland, BT, Dering, K, Duncan, FA, Dunford, M, Erlandson, A, Fatemighomi, N, Fiorillo, G, Flower, A, Ford, RJ, Gagnon, R, Gallacher, D, García Abia, P, Garg, S, Giampa, P, Goeldi, D, Golovko, VV, Gorel, P, Graham, K, Grant, DR, Hallin, AL, Hamstra, M, Harvey, PJ, Hearns, C, Joy, A, Jillings, CJ, Kamaev, O, Kaur, G, Kemp, A, Kochanek, I, Kuźniak, M, Langrock, S, La Zia, F, Lehnert, B, Li, X, Litvinov, O, Lock, J, Longo, G, Majewski, P, McDonald, AB, McElroy, T, McGinn, T, McLaughlin, JB, Mehdiyev, R, Mielnichuk, C, Monroe, J, Nadeau, P, Nantais, C, Ng, C, Noble, AJ, Ouellet, C, Pasuthip, P, Peeters, SJM, Pesudo, V, Piro, MC, Pollmann, TR, Rand, ET, Rethmeier, C, Retière, F, Sanchez García, E, Santorelli, R, Seeburn, N, Skensved, P, Smith, B, Smith, NJT, Sonley, T, Stainforth, R, Stone, C, Strickland, V, Sur, B, Vázquez-Jáuregui, E, Veloce, L, Viel, S, Walding, J, Waqar, M, Ward, M, Westerdale, S, Willis, J, and Zuñiga-Reyes, A

Subjects
nucl-ex, astro-ph.IM
Abstract

The DEAP-3600 experiment is searching for weakly interacting massive particles dark matter with a 3.3 ×103 kg single phase liquid argon (LAr) target, located 2.1 km underground at SNOLAB. The experimental signature of dark matter interactions is kilo electron volt-scale Ar40 nuclear recoils producing 128 nm LAr scintillation photons observed by photomultiplier tubes. The largest backgrounds in DEAP-3600 are electronic recoils (ERs) induced by β and γ rays originating from internal and external radioactivity in the detector material. A background model of the ER interactions in DEAP-3600 was developed and is described in this work. The model is based on several components which are expected from radioisotopes in the LAr, from ex situ material assay measurements, and from dedicated independent in situ analyses. This prior information is used in a Bayesian fit of the ER components to a 247.2 d dataset to model the radioactivity in the surrounding detector materials. Pulse-shape discrimination separates ER and NR events. However, detailed knowledge of the ER background and activity of detector components sets valuable constraints on NR backgrounds including neutrons and alphas. In addition, the activity of Ar42 in LAr in DEAP-3600 is determined by measuring the daughter decay of K42. This cosmogenically activated trace isotope is a relevant background at higher energies for other rare event searches using atmospheric argon, e.g., DarkSide-20k, GERDA, or LEGEND. The specific activity of Ar42 in the atmosphere is found to be 40.4±5.9 μBq/kg of argon.

Published
2019

5. Measurement of neutron production in atmospheric neutrino interactions at the Sudbury Neutrino Observatory

Author

Aharmim, B, Ahmed, SN, Anthony, AE, Barros, N, Beier, EW, Bellerive, A, Beltran, B, Bergevin, M, Biller, SD, Bonventre, R, Boudjemline, K, Boulay, MG, Cai, B, Callaghan, EJ, Caravaca, J, Chan, YD, Chauhan, D, Chen, M, Cleveland, BT, Cox, GA, Dai, X, Deng, H, Descamps, FB, Detwiler, JA, Doe, PJ, Doucas, G, Drouin, P-L, Dunford, M, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Fleurot, F, Ford, RJ, Formaggio, JA, Gagnon, N, Gilje, K, Goon, JTM, Graham, K, Guillian, E, Habib, S, Hahn, RL, Hallin, AL, Hallman, ED, Harvey, PJ, Hazama, R, Heintzelman, WJ, Heise, J, Helmer, RL, Hime, A, Howard, C, Huang, M, Jagam, P, Jamieson, B, Jelley, NA, Jerkins, M, Keeter, KJ, Klein, JR, Kormos, LL, Kos, M, Kruger, A, Kraus, C, Krauss, CB, Kutter, T, Kyba, CCM, Land, BJ, Lange, R, Law, J, Lawson, IT, Lesko, KT, Leslie, JR, Levine, I, Loach, JC, MacLellan, R, Majerus, S, Mak, HB, Maneira, J, Martin, RD, Mastbaum, A, McCauley, N, McDonald, AB, McGee, SR, Miller, ML, Monreal, B, Monroe, J, Nickel, BG, Noble, AJ, O'Keeffe, HM, Oblath, NS, Okada, CE, Ollerhead, RW, Gann, GD Orebi, Oser, SM, Ott, RA, Peeters, SJM, Poon, AWP, Prior, G, Reitzner, SD, and Rielage, K

Subjects
hep-ex
Abstract

Neutron production in GeV-scale neutrino interactions is a poorly studiedprocess. We have measured the neutron multiplicities in atmospheric neutrinointeractions in the Sudbury Neutrino Observatory experiment and compared themto the prediction of a Monte Carlo simulation using GENIE and a minimallymodified version of GEANT4. We analyzed 837 days of exposure corresponding toPhase I, using pure heavy water, and Phase II, using a mixture of Cl in heavywater. Neutrons produced in atmospheric neutrino interactions were identifiedwith an efficiency of $15.3\%$ and $44.3\%$, for Phase I and II respectively.The neutron production is measured as a function of the visible energy of theneutrino interaction and, for charged current quasi-elastic interactioncandidates, also as a function of the neutrino energy. This study is alsoperformed classifying the complete sample into two pairs of event categories:charged current quasi-elastic and non charged current quasi-elastic, and$\nu_{\mu}$ and $\nu_e$. Results show good overall agreement between data andMonte Carlo for both phases, with some small tension with a statisticalsignificance below $2\sigma$ for some intermediate energies.

Published
2019

6. In-situ characterization of the Hamamatsu R5912-HQE photomultiplier tubes used in the DEAP-3600 experiment

Author

Amaudruz, P-A, Batygov, M, Beltran, B, Bina, CE, Bishop, D, Bonatt, J, Boorman, G, Boulay, MG, Broerman, B, Bromwich, T, Bueno, JF, Butcher, A, Cai, B, Chan, S, Chen, M, Chouinard, R, Churchwell, S, Cleveland, BT, Cranshaw, D, Dering, K, Dittmeier, S, Duncan, FA, Dunford, M, Erlandson, A, Fatemighomi, N, Ford, RJ, Gagnon, R, Giampa, P, Golovko, VV, Gorel, P, Gornea, R, Grace, E, Graham, K, Grant, DR, Gulyev, E, Hall, A, Hallin, AL, Hamstra, M, Harvey, PJ, Hearns, C, Jillings, CJ, Kamaev, O, Kemp, A, Kuźniak, M, Langrock, S, La Zia, F, Lehnert, B, Li, O, Lidgard, JJ, Liimatainen, P, Lim, C, Lindner, T, Linn, Y, Liu, S, Mathew, R, McDonald, AB, McElroy, T, McFarlane, K, McLaughlin, J, Mead, S, Mehdiyev, R, Mielnichuk, C, Monroe, J, Muir, A, Nadeau, P, Nantais, C, Ng, C, Noble, AJ, O’Dwyer, E, Ohlmann, C, Olchanski, K, Olsen, KS, Ouellet, C, Pasuthip, P, Peeters, SJM, Pollmann, TR, Rand, ET, Rau, W, Rethmeier, C, Retière, F, Seeburn, N, Shaw, B, Singhrao, K, Skensved, P, Smith, B, Smith, NJT, Sonley, T, Stainforth, R, Stone, C, Strickland, V, Sur, B, Tang, J, Taylor, J, Veloce, L, Vázquez-Jáuregui, E, Walding, J, Ward, M, Westerdale, S, White, R, and Woolsey, E

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, PMT, Hamamatsu R5912-HQE, Single photoelectron charge distribution, Afterpulsing, Late and double pulsing, Dark noise, Dark matter detection, physics.ins-det, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Other Physical Sciences, Nuclear & Particles Physics, Nuclear and plasma physics
Abstract

The Hamamatsu R5912-HQE photomultiplier-tube (PMT) is a novel high-quantum efficiency PMT. It is currently used in the DEAP-3600 dark matter detector and is of significant interest for future dark matter and neutrino experiments where high signal yields are needed. We report on the methods developed for in-situ characterization and monitoring of DEAP's 255 R5912-HQE PMTs. This includes a detailed discussion of typical measured single-photoelectron charge distributions, correlated noise (afterpulsing), dark noise, double, and late pulsing characteristics. The characterization is performed during the detector commissioning phase using laser light injected through a light diffusing sphere and during normal detector operation using LED light injected through optical fibres.

Published
2019

7. In-situ characterization of the Hamamatsu R5912-HQE photomultiplier tubes used in the DEAP-3600 experiment

Author

Amaudruz, PA, Batygov, M, Beltran, B, Bina, CE, Bishop, D, Bonatt, J, Boorman, G, Boulay, MG, Broerman, B, Bromwich, T, Bueno, JF, Butcher, A, Cai, B, Chan, S, Chen, M, Chouinard, R, Churchwell, S, Cleveland, BT, Cranshaw, D, Dering, K, Dittmeier, S, Duncan, FA, Dunford, M, Erlandson, A, Fatemighomi, N, Ford, RJ, Gagnon, R, Giampa, P, Golovko, VV, Gorel, P, Gornea, R, Grace, E, Graham, K, Grant, DR, Gulyev, E, Hall, A, Hallin, AL, Hamstra, M, Harvey, PJ, Hearns, C, Jillings, CJ, Kamaev, O, Kemp, A, Kuźniak, M, Langrock, S, La Zia, F, Lehnert, B, Li, O, Lidgard, JJ, Liimatainen, P, Lim, C, Lindner, T, Linn, Y, Liu, S, Mathew, R, McDonald, AB, McElroy, T, McFarlane, K, McLaughlin, J, Mead, S, Mehdiyev, R, Mielnichuk, C, Monroe, J, Muir, A, Nadeau, P, Nantais, C, Ng, C, Noble, AJ, O'Dwyer, E, Ohlmann, C, Olchanski, K, Olsen, KS, Ouellet, C, Pasuthip, P, Peeters, SJM, Pollmann, TR, Rand, ET, Rau, W, Rethmeier, C, Retière, F, Seeburn, N, Shaw, B, Singhrao, K, Skensved, P, Smith, B, Smith, NJT, Sonley, T, Stainforth, R, Stone, C, Strickland, V, Sur, B, Tang, J, Taylor, J, Veloce, L, Vázquez-Jáuregui, E, Walding, J, Ward, M, Westerdale, S, White, R, and Woolsey, E

Subjects
PMT, Hamamatsu R5912-HQE, Single photoelectron charge distribution, Afterpulsing, Late and double pulsing, Dark noise, Dark matter detection, physics.ins-det, Nuclear & Particles Physics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Other Physical Sciences
Abstract

The Hamamatsu R5912-HQE photomultiplier-tube (PMT) is a novel high-quantum efficiency PMT. It is currently used in the DEAP-3600 dark matter detector and is of significant interest for future dark matter and neutrino experiments where high signal yields are needed. We report on the methods developed for in-situ characterization and monitoring of DEAP's 255 R5912-HQE PMTs. This includes a detailed discussion of typical measured single-photoelectron charge distributions, correlated noise (afterpulsing), dark noise, double, and late pulsing characteristics. The characterization is performed during the detector commissioning phase using laser light injected through a light diffusing sphere and during normal detector operation using LED light injected through optical fibres.

Published
2019

8. Design and construction of the DEAP-3600 dark matter detector

Author

Amaudruz, P-A, Baldwin, M, Batygov, M, Beltran, B, Bina, CE, Bishop, D, Bonatt, J, Boorman, G, Boulay, MG, Broerman, B, Bromwich, T, Bueno, JF, Burghardt, PM, Butcher, A, Cai, B, Chan, S, Chen, M, Chouinard, R, Churchwell, S, Cleveland, BT, Cranshaw, D, Dering, K, DiGioseffo, J, Dittmeier, S, Duncan, FA, Dunford, M, Erlandson, A, Fatemighomi, N, Florian, S, Flower, A, Ford, RJ, Gagnon, R, Giampa, P, Golovko, VV, Gorel, P, Gornea, R, Grace, E, Graham, K, Grant, DR, Gulyev, E, Hall, A, Hallin, AL, Hamstra, M, Harvey, PJ, Hearns, C, Jillings, CJ, Kamaev, O, Kemp, A, Kuźniak, M, Langrock, S, La Zia, F, Lehnert, B, Li, O, Lidgard, JJ, Liimatainen, P, Lim, C, Lindner, T, Linn, Y, Liu, S, Majewski, P, Mathew, R, McDonald, AB, McElroy, T, McFarlane, K, McGinn, T, McLaughlin, JB, Mead, S, Mehdiyev, R, Mielnichuk, C, Monroe, J, Muir, A, Nadeau, P, Nantais, C, Ng, C, Noble, AJ, O’Dwyer, E, Ohlmann, C, Olchanski, K, Olsen, KS, Ouellet, C, Pasuthip, P, Peeters, SJM, Pollmann, TR, Rand, ET, Rau, W, Rethmeier, C, Retière, F, Seeburn, N, Shaw, B, Singhrao, K, Skensved, P, Smith, B, Smith, NJT, Sonley, T, Soukup, J, Stainforth, R, Stone, C, Strickland, V, Sur, B, and Tang, J

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, Dark matter, WIMP, Liquid Argon, DEAP, SNOLAB, Low background, astro-ph.IM, hep-ex, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Astronomical sciences, Particle and high energy physics
Abstract

The Dark matter Experiment using Argon Pulse-shape discrimination (DEAP) has been designed for a direct detection search for particle dark matter using a single-phase liquid argon target. The projected cross section sensitivity for DEAP-3600 to the spin-independent scattering of Weakly Interacting Massive Particles (WIMPs) on nucleons is 10−46cm2 for a 100 GeV/c2 WIMP mass with a fiducial exposure of 3 tonne-years. This paper describes the physical properties and construction of the DEAP-3600 detector.

Published
2019

9. Design and construction of the DEAP-3600 dark matter detector

Author

Amaudruz, PA, Baldwin, M, Batygov, M, Beltran, B, Bina, CE, Bishop, D, Bonatt, J, Boorman, G, Boulay, MG, Broerman, B, Bromwich, T, Bueno, JF, Burghardt, PM, Butcher, A, Cai, B, Chan, S, Chen, M, Chouinard, R, Churchwell, S, Cleveland, BT, Cranshaw, D, Dering, K, DiGioseffo, J, Dittmeier, S, Duncan, FA, Dunford, M, Erlandson, A, Fatemighomi, N, Florian, S, Flower, A, Ford, RJ, Gagnon, R, Giampa, P, Golovko, VV, Gorel, P, Gornea, R, Grace, E, Graham, K, Grant, DR, Gulyev, E, Hall, A, Hallin, AL, Hamstra, M, Harvey, PJ, Hearns, C, Jillings, CJ, Kamaev, O, Kemp, A, Kuźniak, M, Langrock, S, La Zia, F, Lehnert, B, Li, O, Lidgard, JJ, Liimatainen, P, Lim, C, Lindner, T, Linn, Y, Liu, S, Majewski, P, Mathew, R, McDonald, AB, McElroy, T, McFarlane, K, McGinn, T, McLaughlin, JB, Mead, S, Mehdiyev, R, Mielnichuk, C, Monroe, J, Muir, A, Nadeau, P, Nantais, C, Ng, C, Noble, AJ, O'Dwyer, E, Ohlmann, C, Olchanski, K, Olsen, KS, Ouellet, C, Pasuthip, P, Peeters, SJM, Pollmann, TR, Rand, ET, Rau, W, Rethmeier, C, Retière, F, Seeburn, N, Shaw, B, Singhrao, K, Skensved, P, Smith, B, Smith, NJT, Sonley, T, Soukup, J, Stainforth, R, Stone, C, Strickland, V, Sur, B, and Tang, J

Subjects
Dark matter, WIMP, Liquid Argon, DEAP, SNOLAB, Low background, astro-ph.IM, hep-ex, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics
Abstract

The Dark matter Experiment using Argon Pulse-shape discrimination (DEAP) has been designed for a direct detection search for particle dark matter using a single-phase liquid argon target. The projected cross section sensitivity for DEAP-3600 to the spin-independent scattering of Weakly Interacting Massive Particles (WIMPs) on nucleons is 10−46cm2 for a 100 GeV/c2 WIMP mass with a fiducial exposure of 3 tonne-years. This paper describes the physical properties and construction of the DEAP-3600 detector.

Published
2019

10. Constraints on neutrino lifetime from the Sudbury Neutrino Observatory

Author

Aharmim, B, Ahmed, SN, Anthony, AE, Barros, N, Beier, EW, Bellerive, A, Beltran, B, Bergevin, M, Biller, SD, Bonventre, R, Boudjemline, K, Boulay, MG, Cai, B, Callaghan, EJ, Caravaca, J, Chan, YD, Chauhan, D, Chen, M, Cleveland, BT, Cox, GA, Dai, X, Deng, H, Descamps, FB, Detwiler, JA, Doe, PJ, Doucas, G, Drouin, P-L, Dunford, M, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Fleurot, F, Ford, RJ, Formaggio, JA, Gagnon, N, Gilje, K, Goon, J TM, Graham, K, Guillian, E, Habib, S, Hahn, RL, Hallin, AL, Hallman, ED, Harvey, PJ, Hazama, R, Heintzelman, WJ, Heise, J, Helmer, RL, Hime, A, Howard, C, Huang, M, Jagam, P, Jamieson, B, Jelley, NA, Jerkins, M, Kéfélian, C, Keeter, KJ, Klein, JR, Kormos, LL, Kos, M, Krüger, A, Kraus, C, Krauss, CB, Kutter, T, Kyba, CCM, Land, BJ, Lange, R, Law, J, Lawson, IT, Lesko, KT, Leslie, JR, Levine, I, Loach, JC, MacLellan, R, Majerus, S, Mak, HB, Maneira, J, Martin, RD, Mastbaum, A, McCauley, N, McDonald, AB, McGee, SR, Miller, ML, Monreal, B, Monroe, J, Nickel, BG, Noble, AJ, O’Keeffe, HM, Oblath, NS, Okada, CE, Ollerhead, RW, Gann, GD Orebi, Oser, SM, Ott, RA, Peeters, SJM, Poon, AWP, Prior, G, and Reitzner, SD

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, hep-ex, nucl-ex
Abstract

The long baseline between Earth and the Sun makes solar neutrinos an excellent test beam for exploring possible neutrino decay. The signature of such decay would be an energy-dependent distortion of the traditional survival probability which can be fit for using well-developed and high-precision analysis methods. Here a model including neutrino decay is fit to all three phases of B8 solar neutrino data taken by the Sudbury Neutrino Observatory (SNO). This fit constrains the lifetime of neutrino mass state ν2 to be >8.08×10-5 s/eV at 90% confidence. An analysis combining this SNO result with those from other solar neutrino experiments results in a combined limit for the lifetime of mass state ν2 of >1.92×10-3 s/eV at 90% confidence.

Published
2019

11. Tests of Lorentz invariance at the Sudbury Neutrino Observatory

Author

Aharmim, B, Ahmed, SN, Anthony, AE, Barros, N, Beier, EW, Bellerive, A, Beltran, B, Bergevin, M, Biller, SD, Blucher, E, Bonventre, R, Boudjemline, K, Boulay, MG, Cai, B, Callaghan, EJ, Caravaca, J, Chan, YD, Chauhan, D, Chen, M, Cleveland, BT, Cox, GA, Dai, X, Deng, H, Descamps, FB, Detwiler, JA, Doe, PJ, Doucas, G, Drouin, P-L, Dunford, M, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Fleurot, F, Ford, RJ, Formaggio, JA, Gagnon, N, Gilje, K, Goon, J TM, Graham, K, Guillian, E, Habib, S, Hahn, RL, Hallin, AL, Hallman, ED, Harvey, PJ, Hazama, R, Heintzelman, WJ, Heise, J, Helmer, RL, Hime, A, Howard, C, Huang, M, Jagam, P, Jamieson, B, Jelley, NA, Jerkins, M, Kéfélian, C, Keeter, KJ, Klein, JR, Kormos, LL, Kos, M, Krüger, A, Kraus, C, Krauss, CB, Kutter, T, Kyba, CCM, Labe, K, Land, BJ, Lange, R, LaTorre, A, Law, J, Lawson, IT, Lesko, KT, Leslie, JR, Levine, I, Loach, JC, MacLellan, R, Majerus, S, Mak, HB, Maneira, J, Martin, RD, Mastbaum, A, McCauley, N, McDonald, AB, McGee, SR, Miller, ML, Monreal, B, Monroe, J, Nickel, BG, Noble, AJ, O’Keeffe, HM, Oblath, NS, Okada, CE, Ollerhead, RW, Gann, GD Orebi, Oser, SM, Ott, RA, and Peeters, SJM

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, hep-ex, nucl-ex
Abstract

Experimental tests of Lorentz symmetry in systems of all types are critical for ensuring that the basic assumptions of physics are well founded. Data from all phases of the Sudbury Neutrino Observatory, a kiloton-scale heavy water Cherenkov detector, are analyzed for possible violations of Lorentz symmetry in the neutrino sector. Such violations would appear as one of eight possible signal types in the detector: six seasonal variations in the solar electron neutrino survival probability differing in energy and time dependence and two shape changes to the oscillated solar neutrino energy spectrum. No evidence for such signals is observed, and limits on the size of such effects are established in the framework of the standard model extension, including 38 limits on previously unconstrained operators and improved limits on 16 additional operators. This makes limits on all minimal, Dirac-type Lorentz violating operators in the neutrino sector available for the first time.

Published
2018

12. Search for neutron-Antineutron oscillations at the Sudbury Neutrino Observatory

Author

Aharmim, B, Ahmed, SN, Anthony, AE, Barros, N, Beier, EW, Bellerive, A, Beltran, B, Bergevin, M, Biller, SD, Boudjemline, K, Boulay, MG, Cai, B, Chan, YD, Chauhan, D, Chen, M, Cleveland, BT, Cox, GA, Dai, X, Deng, H, Detwiler, JA, Doe, PJ, Doucas, G, Drouin, PL, Duncan, FA, Dunford, M, Earle, ED, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Fleurot, F, Ford, RJ, Formaggio, JA, Gagnon, N, Goon, JT, Graham, K, Guillian, E, Habib, S, Hahn, RL, Hallin, AL, Hallman, ED, Harvey, PJ, Hazama, R, Heintzelman, WJ, Heise, J, Helmer, RL, Hime, A, Howard, C, Huang, M, Jagam, P, Jamieson, B, Jelley, NA, Jerkins, M, Keeter, KJ, Klein, JR, Kormos, LL, Kos, M, Krüger, A, Kraus, C, Krauss, CB, Kutter, T, Kyba, CCM, Lange, R, Law, J, Lawson, IT, Lesko, KT, Leslie, JR, Levine, I, Loach, JC, Maclellan, R, Majerus, S, Mak, HB, Maneira, J, Martin, RD, McCauley, N, McDonald, AB, McGee, SR, Miller, ML, Monreal, B, Monroe, J, Nickel, BG, Noble, AJ, O'Keeffe, HM, Oblath, NS, Okada, CE, Ollerhead, RW, Orebi Gann, GD, Oser, SM, Ott, RA, Peeters, SJM, Poon, AWP, Prior, G, Reitzner, SD, Rielage, K, Robertson, BC, Robertson, RGH, Schwendener, MH, Secrest, JA, and Seibert, SR

Subjects
hep-ex, nucl-ex, physics.ins-det
Abstract

Tests on B-L symmetry breaking models are important probes to search for new physics. One proposed model with Δ(B-L)=2 involves the oscillations of a neutron to an antineutron. In this paper, a new limit on this process is derived for the data acquired from all three operational phases of the Sudbury Neutrino Observatory experiment. The search concentrated on oscillations occurring within the deuteron, and 23 events were observed against a background expectation of 30.5 events. These translated to a lower limit on the nuclear lifetime of 1.48×1031 yr at 90% C.L. when no restriction was placed on the signal likelihood space (unbounded). Alternatively, a lower limit on the nuclear lifetime was found to be 1.18×1031 yr at 90% C.L. when the signal was forced into a positive likelihood space (bounded). Values for the free oscillation time derived from various models are also provided in this article. This is the first search for neutron-Antineutron oscillation with the deuteron as a target.

Published
2017

13. Light Sterile Neutrinos: A White Paper

Author

Abazajian, KN, Acero, MA, Agarwalla, SK, Aguilar-Arevalo, AA, Albright, CH, Antusch, S, Arguelles, CA, Balantekin, AB, Barenboim, G, Barger, V, Bernardini, P, Bezrukov, F, Bjaelde, OE, Bogacz, SA, Bowden, NS, Boyarsky, A, Bravar, A, Berguno, D Bravo, Brice, SJ, Bross, AD, Caccianiga, B, Cavanna, F, Chun, EJ, Cleveland, BT, Collin, AP, Coloma, P, Conrad, JM, Cribier, M, Cucoanes, AS, D'Olivo, JC, Das, S, Gouvea, A de, Derbin, AV, Dharmapalan, R, Diaz, JS, Ding, XJ, Djurcic, Z, Donini, A, Duchesneau, D, Ejiri, H, Elliott, SR, Ernst, DJ, Esmaili, A, Evans, JJ, Fernandez-Martinez, E, Figueroa-Feliciano, E, Fleming, BT, Formaggio, JA, Franco, D, Gaffiot, J, Gandhi, R, Gao, Y, Garvey, GT, Gavrin, VN, Ghoshal, P, Gibin, D, Giunti, C, Gninenko, SN, Gorbachev, VV, Gorbunov, DS, Guenette, R, Guglielmi, A, Halzen, F, Hamann, J, Hannestad, S, Haxton, W, Heeger, KM, Henning, R, Hernandez, P, Huber, P, Huelsnitz, W, Ianni, A, Ibragimova, TV, Karadzhov, Y, Karagiorgi, G, Keefer, G, Kim, YD, Kopp, J, Kornoukhov, VN, Kusenko, A, Kyberd, P, Langacker, P, Lasserre, Th, Laveder, M, Letourneau, A, Lhuillier, D, Li, YF, Lindner, M, Link, JM, Littlejohn, BL, Lombardi, P, Long, K, Lopez-Pavon, J, Louis, WC, Ludhova, L, Lykken, JD, Machado, PAN, Maltoni, M, Mann, WA, and Marfatia, D

Subjects
hep-ph, astro-ph.CO, hep-ex, nucl-ex, nucl-th
Abstract

This white paper addresses the hypothesis of light sterile neutrinos based onrecent anomalies observed in neutrino experiments and the latest astrophysicaldata.

Published
2012

14. Recent Results from SNO

Author

Sinclair, D, Kutter, T, Nally, CW, Oser, SM, Waltham, CE, Boger, J, Hahn, RL, Lange, R, Yeh, M, Bellerive, A, Dai, X, Dalnoki-Veress, F, Dosanjh, RS, Grant, DR, Hargrove, CK, Hemingway, RJ, Levine, I, Mifflin, C, Rollin, E, Simard, O, Starinsky, N, Tesic, G, Waller, D, Jagam, P, Labranche, H, Law, J, Lawson, IT, Nickel, BG, Ollerhead, RW, Simpson, JJ, Farine, J, Fleurot, F, Hallman, ED, Luoma, S, Schwendener, MH, Tafirout, R, Virtue, CJ, Chan, YD, Chen, X, Heeger, KM, Lesko, KT, Marino, AD, Norman, EB, Okada, CE, Poon, AWP, Rosendahl, SSE, Stokstad, RG, Boulay, MG, Bowles, TJ, Brice, SJ, Dragowsky, MR, Elliott, SR, Fowler, MM, Hamer, AS, Heise, J, Hime, A, Miller, GG, Van de Water, RG, Wilhelmy, JB, Wouters, JM, Biller, SD, Bowler, MG, Cleveland, BT, Doucas, G, Dunmore, JA, Fergani, H, Frame, K, Jelley, NA, Majerus, S, McGregor, G, Peeters, SJM, Sims, CJ, Thorman, M, Tseung, HWC, West, N, Wilson, JR, Zuber, K, Beier, EW, Dunford, M, Heintzelman, WJ, Kyba, CCM, McCauley, N, Rusu, VL, Van Berg, R, Ahmed, SN, Chen, M, Duncan, FA, Earle, ED, Fulsom, BG, Evans, HC, Ewan, GT, Graham, K, Hallin, AL, Handler, WB, Harvey, PJ, Kos, MS, Krumins, AV, Leslie, JR, and MacLellan, R

Subjects
Heavy water, chemistry.chemical_classification, Nuclear and High Energy Physics, chemistry.chemical_compound, Materials science, chemistry, Seesaw molecular geometry, Chemical engineering, Phase (matter), Salt (chemistry), Nanotechnology, Atomic and Molecular Physics, and Optics
Abstract

The SNO project has now completed two of its three major phases of operation. The no-oscillation hypothesis has been ruled out at 5σ in the pure heavy water phase and 8σ in the salt phase. Discussion in terms of the SeeSaw model is presented. © 2004 Published by Elsevier B.V.

Published
2004

15. Determination of the nu(e) and total B-8 solar neutrino fluxes using the Sudbury Neutrino Observatory Phase I data set

Author

Aharmim, B, Ahmad, QR, Ahmed, SN, Allen, RC, Andersen, TC, Anglin, JD, Buehler, G, Barton, JC, Beier, EW, Bercovitch, M, Bergevin, M, Bigu, J, Biller, SD, Black, RA, Blevis, I, Boardman, RJ, Boger, J, Bonvin, E, Boulay, MG, Bowler, MG, Bowles, TJ, Brice, SJ, Browne, MC, Bullard, TV, Burritt, TH, Cameron, J, Chan, YD, Chen, HH, Chen, M, Chen, X, Cleveland, BT, Cowan, JHM, Cowen, DF, Cox, GA, Currat, CA, Dai, X, Dalnoki-Veress, F, Davidson, WF, Deng, H, DiMarco, M, Doe, PJ, Doucas, G, Dragowsky, MR, Duba, CA, Duncan, FA, Dunford, M, Dunmore, JA, Earle, ED, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Ferraris, AP, Fleurot, F, Ford, RJ, Formaggio, JA, Fowler, MM, Frame, K, Frank, ED, Frati, W, Gagnon, N, Germani, JV, Gil, S, Goldschmidt, A, Goon, JTM, Graham, K, Grant, DR, Guillian, E, Hahn, RL, Hallin, AL, Hallman, ED, Hamer, AS, Hamian, AA, Handler, WB, Haq, RU, Hargrove, CK, Harvey, PJ, Hazama, R, Heeger, KM, Heintzelman, WJ, Heise, J, Helmer, RL, Henning, R, Hepburn, JD, Heron, H, Hewett, J, Hime, A, Howard, C, Howe, MA, Huang, M, Hykaway, JG, Isaac, MCP, Jagam, P, Jamieson, B, Jelley, NA, Jillings, C, Jonkmans, G, Kazkaz, K, Keener, PT, Kirch, K, Klein, JR, Knox, AB, Komar, RJ, Kormos, LL, Kos, M, Kouzes, R, Krueger, A, Kraus, C, Krauss, CB, Kutter, T, Kyba, CCM, Labranche, H, Lange, R, Law, J, Lawson, IT, Lay, M, Lee, HW, Lesko, KT, Leslie, JR, Levine, I, Loach, JC, Locke, W, Luoma, S, Lyon, J, MacLellan, R, Majerus, S, Mak, HB, Maneira, J, Marino, AD, Martin, R, McCauley, N, McDonald, AB, McDonald, DS, McFarlane, K, McGee, S, McGregor, G, Drees, RM, Mes, H, Mifflin, C, Miknaitis, KKS, Miller, ML, Milton, G, Moffat, BA, Monreal, B, Moorhead, M, Morrissette, B, Nally, CW, Neubauer, MS, Newcomer, FM, Ng, HS, Nickel, BG, Noble, AJ, Norman, EB, Novikov, VM, Oblath, NS, Okada, CE, O'Keeffe, HM, Ollerhead, RW, Omori, M, Orrell, JL, Oser, SM, Ott, R, Peeters, SJM, Poon, AWP, Prior, G, Reitzner, SD, Rielage, K, Roberge, A, Robertson, BC, Robertson, RGH, Rosendahl, SSE, Rowley, JK, Rusu, VL, Saettler, E, Schulke, A, Schwendener, MH, Secrest, JA, Seifert, H, Shatkay, M, Simpson, JJ, Sims, CJ, Sinclair, D, Skensved, P, Smith, AR, Smith, MWE, Starinsky, N, Steiger, TD, Stokstad, RG, Stonehill, LC, Storey, RS, Sur, B, Tafirout, R, Tagg, N, Takeuchi, Y, Tanner, NW, Taplin, RK, Thorman, M, Thornewell, PM, Tolich, N, Trent, PT, Tserkovnyak, YI, Tsui, T, Tunnell, CD, Van Berg, R, De Water, RGV, Virtue, CJ, Walker, TJ, Wall, BL, Waltham, CE, Tseung, HWC, Wang, J-X, Wark, DL, Wendland, J, West, N, Wilhelmy, JB, Wilkerson, JF, Wilson, JR, Wittich, P, Wouters, JM, Wright, A, Yeh, M, Zuber, K, and Collaboration, SNO

Published
2007

16. Electron energy spectra, fluxes, and day-night asymmetries of B-8 solar neutrinos from measurements with NaCl dissolved in the heavy-water detector at the Sudbury Neutrino Observatory

Author

Aharmim, B, Ahmed, SN, Anthony, AE, Beier, EW, Bellerive, A, Bergevin, M, Biller, SD, Boger, J, Boulay, MG, Bowler, MG, Bullard, TV, Chan, YD, Chen, M, Chen, X, Cleveland, BT, Cox, GA, Currat, CA, Dai, X, Dalnoki-Veress, F, Deng, H, Doe, PJ, Dosanjh, RS, Doucas, G, Duba, CA, Duncan, FA, Dunford, M, Dunmore, JA, Earle, ED, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Fleurot, F, Formaggio, JA, Frame, K, Frati, W, Fulsom, BG, Gagnon, N, Graham, K, Grant, DR, Hahn, RL, Hall, JC, Hallin, AL, Hallman, ED, Handler, WB, Hargrove, CK, Harvey, PJ, Hazama, R, Heeger, KM, Heelan, L, Heintzelman, WJ, Heise, J, Helmer, RL, Hemingway, RJ, Hime, A, Howard, C, Howe, MA, Huang, M, Jagam, P, Jelley, NA, Klein, JR, Kormos, LL, Kos, MS, Kruger, A, Kraus, C, Krauss, CB, Krumins, AV, Kutter, T, Kyba, CCM, Labranche, H, Lange, R, Law, J, Lawson, IT, Lesko, KT, Leslie, JR, Levine, I, Loach, JC, Luoma, S, MacLellan, R, Majerus, S, Mak, HB, Maneira, J, Marino, AD, McCauley, N, McDonald, AB, McGee, S, McGregor, G, Mifflin, C, Miknaitis, KKS, Moffat, BA, Nally, CW, Neubauer, MS, Nickel, BG, Noble, AJ, Norman, EB, Oblath, NS, Okada, CE, Ollerhead, RW, Orrell, JL, Oser, SM, Ouellet, C, Peeters, SJM, Poon, AWP, Rielage, K, Robertson, BC, Robertson, RGH, Rollin, E, Rosendahl, SSE, Rusu, VL, Schwendener, MH, Seibert, SR, Simard, O, Simpson, JJ, Sims, CJ, Sinclair, D, Skensved, P, Smith, MWE, Starinsky, N, Stokstad, RG, Stonehill, LC, Tafirout, R, Takeuchi, Y, Tesic, G, Thomson, M, Thorman, M, Tsui, T, Van Berg, R, Van de Water, RG, Virtue, CJ, Wall, BL, Waller, D, Waltham, CE, Tseung, HWC, Wark, DL, Wendland, J, West, N, Wilkerson, JF, Wilson, JR, Wittich, P, Wouters, JM, Wright, A, Yeh, M, Zuber, K, and Collaboration, SNO

Subjects
High Energy Physics::Experiment, Astrophysics::Cosmology and Extragalactic Astrophysics, Nuclear Experiment
Abstract

Results are reported from the complete salt phase of the Sudbury Neutrino Observatory experiment in which NaCl was dissolved in the H22O ("D2O") target. The addition of salt enhanced the signal from neutron capture as compared to the pure D2O detector. By making a statistical separation of charged-current events from other types based on event-isotropy criteria, the effective electron recoil energy spectrum has been extracted. In units of 106cm-2s-1, the total flux of active-flavor neutrinos from B8 decay in the Sun is found to be 4.94-0.21+0.21(stat)-0.34+0.38(syst) and the integral flux of electron neutrinos for an undistorted B8 spectrum is 1.68-0.06+0.06(stat)-0. 09+0.08(syst); the signal from (νx,e) elastic scattering is equivalent to an electron-neutrino flux of 2.35-0.22+0.22(stat)-0.15+0.15(syst). These results are consistent with those expected for neutrino oscillations with the so-called large mixing angle parameters and also with an undistorted spectrum. A search for matter-enhancement effects in the Earth through a possible day-night asymmetry in the charged-current integral rate is consistent with no asymmetry. Including results from other experiments, the best-fit values for two-neutrino mixing parameters are Δm2=(8.0-0.4+0.6)×10-5 eV2 and θ=33.9-2.2+2.4 degrees. © 2005 The American Physical Society.

Published
2005

17. Search for periodicities in the B8 solar neutrino flux measured by the Sudbury Neutrino Observatory

Author

Aharmim, B, Ahmed, SN, Anthony, AE, Beier, EW, Bellerive, A, Bergevin, M, Biller, SD, Boulay, MG, Bowler, MG, Chan, YD, Chen, M, Chen, X, Cleveland, BT, Costin, T, Cox, GA, Currat, CA, Dai, X, Deng, H, Detwiler, J, Doe, PJ, Dosanjh, RS, Doucas, G, Duba, CA, Duncan, FA, Dunford, M, Dunmore, JA, Earle, ED, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Fleurot, F, Formaggio, JA, Frati, W, Fulsom, BG, Gagnon, N, Goon, JTM, Graham, K, Hahn, RL, Hallin, AL, Hallman, ED, Handler, WB, Hargrove, CK, Harvey, PJ, Hazama, R, Heeger, KM, Heelan, L, Heintzelman, WJ, Heise, J, Helmer, RL, Hemingway, RJ, Hime, A, Howe, MA, Huang, M, Inrig, E, Jagam, P, Jelley, NA, Klein, JR, Kormos, LL, Kos, MS, Krüger, A, Kraus, C, Krauss, CB, Krumins, AV, Kutter, T, Kyba, CCM, Labranche, H, Lange, R, Law, J, Lawson, IT, Lesko, KT, Leslie, JR, Levine, I, Loach, JC, Luoma, S, MacLellan, R, Majerus, S, Maneira, J, Marino, AD, McCauley, N, McDonald, AB, McGee, S, Mifflin, C, Miknaitis, KKS, Nickel, BG, Noble, AJ, Norman, EB, Oblath, NS, Okada, CE, O'Keeffe, HM, Ollerhead, RW, Gann, GDO, Orrell, JL, Oser, SM, Ouvarova, T, Peeters, SJM, Poon, AWP, Pun, CSJ, Rielage, K, Robertson, BC, Robertson, RGH, Rollin, E, Rosendahl, SSE, Schwendener, MH, Seibert, SR, Simard, O, Simpson, JJ, Sims, CJ, Sinclair, D, Sinclair, L, Skensved, P, Smith, MWE, Stokstad, RG, Stonehill, LC, Tafirout, R, Takeuchi, Y, Tešić, G, Thomson, M, Tsang, KV, Tsui, T, Berg, RV, Virtue, CJ, Wall, BL, Waller, D, Waltham, CE, Tseung, HWC, Wark, DL, Wendland, J, West, N, Wilkerson, JF, Wilson, JR, Wouters, JM, Yeh, M, and Zuber, K

Subjects
Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Experiment
Abstract

A search has been made for sinusoidal periodic variations in the B8 solar neutrino flux using data collected by the Sudbury Neutrino Observatory over a 4-year time interval. The variation at a period of 1 yr is consistent with modulation of the B8 neutrino flux by the Earth's orbital eccentricity. No significant sinusoidal periodicities are found with periods between 1 d and 10 years with either an unbinned maximum likelihood analysis or a Lomb-Scargle periodogram analysis. The data are inconsistent with the hypothesis that the results of the recent analysis by Sturrock et al., based on elastic scattering events in Super-Kamiokande, can be attributed to a 7% sinusoidal modulation of the total B8 neutrino flux. © 2005 The American Physical Society.

Published
2005

18. Search for periodicities in the B-8 solar neutrino flux measured by the Sudbury Neutrino Observatory

Author

Aharmim, B, Ahmed, SN, Anthony, AE, Beier, EW, Bellerive, A, Bergevin, M, Biller, SD, Boulay, MG, Bowler, MG, Chan, YD, Chen, M, Chen, X, Cleveland, BT, Costin, T, Cox, GA, Currat, CA, Dai, X, Deng, H, Detwiler, J, Doe, PJ, Dosanjh, RS, Doucas, G, Duba, CA, Duncan, FA, Dunford, M, Dunmore, JA, Earle, ED, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Fleurot, F, Formaggio, JA, Frati, W, Fulsom, BG, Gagnon, N, Goon, JT, Graham, K, Hahn, RL, Hallin, AL, Hallman, ED, Handler, WB, Hargrove, CK, Harvey, PJ, Hazama, R, Heeger, KM, Heelan, L, Heintzelman, WJ, Heise, J, Helmer, RL, Hemingway, RJ, Hime, A, Howe, MA, Huang, M, Inrig, E, Jagam, P, Jelley, NA, Klein, JR, Kormos, LL, Kos, MS, Kruger, A, Kraus, C, Krauss, CB, Krumins, AV, Kutter, T, Kyba, CCM, Labranche, H, Lange, R, Law, J, Lawson, IT, Lesko, KT, Leslie, JR, Levine, I, Loach, JC, Luoma, S, MacLellan, R, Majerus, S, Maneira, J, Marino, AD, McCauley, N, McDonald, AB, McGee, S, Mifflin, C, Miknaitis, KKS, Nickel, BG, Noble, AJ, Norman, EB, Oblath, NS, Okada, CE, O'Keeffe, HM, Ollerhead, RW, Gann, GDO, Orrell, JL, Oser, SM, Ouvarova, T, Peeters, SJM, Poon, AWP, Pun, CSJ, Rielage, K, Robertson, BC, Robertson, RGH, Rollin, E, Rosendahl, SSE, Schwendener, MH, Seibert, SR, Simard, O, Simpson, JJ, Sims, CJ, Sinclair, D, Sinclair, L, Skensved, P, Smith, MWE, Stokstad, RG, Stonehill, LC, Tafirout, R, Takeuchi, Y, Tesic, G, Thomson, M, Tsang, KV, Tsui, T, Van Berg, R, Virtue, CJ, Wall, BL, Waller, D, Waltham, CE, Tseung, HWC, Wark, DL, Wendland, J, West, N, Wilkerson, JF, Wilson, JR, Wouters, JM, Yeh, M, Zuber, K, and Collaboration, SNO

Published
2005

19. Measurement of Rn-222 dissolved in water at the Sudbury neutrino observatory

Author

Blevis, I, Boger, J, Bonvin, E, Cleveland, BT, Dai, X, Dalnoki-Veress, F, Doucas, G, Farine, J, Fergani, H, Grant, D, Hahn, RL, Hamer, AS, Hargrove, CK, Heron, H, Jagam, P, Jelley, NA, Jillings, C, Knox, AB, Lee, HW, Levine, I, Liu, M, Majerus, S, McDonald, A, McFarlane, K, Mifflin, C, Noble, AJ, Noel, S, Novikov, VM, Rowley, JK, Shatkay, M, Simpson, JJ, Sinclair, D, Sur, B, Wang, JX, Yeh, M, and Zhu, X

Abstract

The technique used at the Sudbury Neutrino Observatory (SNO) to measure the concentration of 222Rn in water is described. Water from the SNO detector is passed through a vacuum degasser (in the light water system) or a membrane contact degasser (in the heavy water system) where dissolved gases, including radon, are liberated. The degasser is connected to a vacuum system which collects the radon on a cold trap and removes most other gases, such as water vapor and N2. After roughly 0.5 tonnes of H2O or 6 tonnes of D2O have been sampled, the accumulated radon is transferred to a Lucas cell. The cell is mounted on a photomultiplier tube which detects the α-particles from the decay of 222Rn and its progeny. The overall degassing and concentration efficiency is about 38% and the single-α counting efficiency is approximately 75%. The sensitivity of the radon assay system for D2O is equivalent to ∼ 3 × 10-15 g U/g water. The radon concentration in both the H 2O and D2O is sufficiently low that the rate of background events from U-chain elements is a small fraction of the interaction rate of solar neutrinos by the neutral current reaction. © 2003 Elsevier B.V. All rights reserved.

Published
2004

20. Measurement of the rate of nu(e) + d --p + p + e(-) interactions produced by (8)B solar neutrinos at the Sudbury Neutrino Observatory

Author

Ahmad, QR, Allen, RC, Andersen, TC, Anglin, JD, Bühler, G, Barton, JC, Beier, EW, Bercovitch, M, Bigu, J, Biller, S, Black, RA, Blevis, I, Boardman, RJ, Boger, J, Bonvin, E, Boulay, MG, Bowler, MG, Bowles, TJ, Brice, SJ, Browne, MC, Bullard, TV, Burritt, TH, Cameron, K, Cameron, J, Chan, YD, Chen, M, Chen, HH, Chen, X, Chon, MC, Cleveland, BT, Clifford, ET, Cowan, JH, Cowen, DF, Cox, GA, Dai, Y, Dai, X, Dalnoki-Veress, F, Davidson, WF, Doe, PJ, Doucas, G, Dragowsky, MR, Duba, CA, Duncan, FA, Dunmore, J, Earle, ED, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Ferraris, AP, Ford, RJ, Fowler, MM, Frame, K, Frank, ED, Frati, W, Germani, JV, Gil, S, Goldschmidt, A, Grant, DR, Hahn, RL, Hallin, AL, Hallman, ED, Hamer, A, Hamian, AA, Haq, RU, Hargrove, CK, Harvey, PJ, Hazama, R, Heaton, R, Heeger, KM, Heintzelman, WJ, Heise, J, Helmer, RL, Hepburn, JD, Heron, H, Hewett, J, Hime, A, Howe, M, Hykawy, JG, Isaac, MC, Jagam, P, Jelley, NA, Jillings, C, Jonkmans, G, Karn, J, Keener, PT, Kirch, K, Klein, JR, Knox, AB, Komar, RJ, Kouzes, R, Kutter, T, Kyba, CC, Law, J, Lawson, IT, Lay, M, Lee, HW, Lesko, KT, Leslie, JR, Levine, I, Locke, W, Lowry, MM, Luoma, S, Lyon, J, Majerus, S, Mak, HB, Marino, AD, McCauley, N, McDonald, AB, McDonald, DS, McFarlane, K, McGregor, G, McLatchie, W, Meijer Drees, R, Mes, H, Mifflin, C, Miller, GG, Milton, G, Moffat, BA, Moorhead, M, Nally, CW, Neubauer, MS, Newcomer, FM, Ng, HS, Noble, AJ, Norman, EB, Novikov, VM, O'Neill, M, Okada, CE, Ollerhead, RW, Omori, M, Orrell, JL, Oser, SM, Poon, AW, Radcliffe, TJ, Roberge, A, Robertson, BC, Robertson, RG, Rowley, JK, Rusu, VL, Saettler, E, Schaffer, KK, Schuelke, A, Schwendener, MH, Seifert, H, Shatkay, M, Simpson, JJ, Sinclair, D, Skensved, P, Smith, AR, Smith, MW, Starinsky, N, Steiger, TD, Stokstad, RG, Storey, RS, Sur, B, Tafirout, R, Tagg, N, Tanner, NW, Taplin, RK, Thorman, M, Thornewell, P, Trent, PT, Tserkovnyak, YI, Van Berg, R, Van de Water, RG, Virtue, CJ, Waltham, CE, Wang, JX, Wark, DL, West, N, Wilhelmy, JB, Wilkerson, JF, Wilson, J, Wittich, P, Wouters, JM, and Yeh, M

Subjects
High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics
Abstract

Solar neutrinos from (8)B decay have been detected at the Sudbury Neutrino Observatory via the charged current (CC) reaction on deuterium and the elastic scattering (ES) of electrons. The flux of nu(e)'s is measured by the CC reaction rate to be straight phi(CC)(nu(e)) = 1.75 +/- 0.07(stat)(+0.12)(-0.11)(syst) +/- 0.05(theor) x 10(6) cm(-2) s(-1). Comparison of straight phi(CC)(nu(e)) to the Super-Kamiokande Collaboration's precision value of the flux inferred from the ES reaction yields a 3.3 sigma difference, assuming the systematic uncertainties are normally distributed, providing evidence of an active non- nu(e) component in the solar flux. The total flux of active 8B neutrinos is determined to be 5.44+/-0.99 x 10(6) cm(-2) s(-1).

Published
2001

21. Results from SAGE

Author

Dzhonrid Abdurashitov, Gavrin, Vn, Girin, Sv, Gorbatchev, Vv, Gusev, Ao, Kalikhov, Av, Knodel, Tv, Mirmov, In, Pshukov, Am, Shalagin, Am, Shikhin, Aa, Veretenkin, Ep, Vermul, Vm, Yants, V., Zatsepin, Gt, Bowles, Tj, Nico, Js, Teasdale, Wa, Wark, Dl, Elliott, Sr, Wilkerson, Jf, Cleveland, Bt, Daily, T., Davis, R., Lande, K., Lee, Ck, Wildenhain, Pw, and Cherry, Ml

Subjects
Nuclear and High Energy Physics, Atomic and Molecular Physics, and Optics

22. THE SOVIET-AMERICAN GALLIUM EXPERIMENT AT BAKSAN A STATUS-REPORT

Author

Abazov, Ai, Abdurashitov, Dn, Anosov, Ol, Danshin, Sn, Eroshkina, La, Faizov, El, Gavrin, Vn, Kalikhov, Av, Knodel, Tv, Knyshenko, Ii, Kornoukhov, Vn, Mezentseva, Sa, Mirmov, In, Ostrinsky, Ai, Petukhov, Vv, Pshukov, Am, Revzin, Ny, Shikhin, Aa, Slyusareva, Yd, Timofeyev, Pv, Veretenkin, Ep, Vermul, Vm, Yantz, Ve, Zakharov, Y., Zatsepin, Gt, Zhandarov, Vi, Bowles, Tj, Cleveland, Bt, Elliott, Sr, Obrien, Ha, Wark, Dl, John Wilkerson, Davis, R., Lande, K., Cherry, Ml, and Kouzes, Rt

23. First Direct Detection Constraints on Planck-Scale Mass Dark Matter with Multiple-Scatter Signatures Using the DEAP-3600 Detector.

Author

Adhikari P, Ajaj R, Alpízar-Venegas M, Auty DJ, Benmansour H, Bina CE, Bonivento W, Boulay MG, Cadeddu M, Cai B, Cárdenas-Montes M, Cavuoti S, Chen Y, Cleveland BT, Corning JM, Daugherty S, DelGobbo P, Di Stefano P, Doria L, Dunford M, Ellingwood E, Erlandson A, Farahani SS, Fatemighomi N, Fiorillo G, Gallacher D, García Abia P, Garg S, Giampa P, Goeldi D, Gorel P, Graham K, Grobov A, Hallin AL, Hamstra M, Hugues T, Ilyasov A, Joy A, Jigmeddorj B, Jillings CJ, Kamaev O, Kaur G, Kemp A, Kochanek I, Kuźniak M, Lai M, Langrock S, Lehnert B, Leonhardt A, Levashko N, Li X, Lissia M, Litvinov O, Lock J, Longo G, Machulin I, McDonald AB, McElroy T, McLaughlin JB, Mielnichuk C, Mirasola L, Monroe J, Oliviéro G, Pal S, Peeters SJM, Perry M, Pesudo V, Picciau E, Piro MC, Pollmann TR, Raj N, Rand ET, Rethmeier C, Retière F, Rodríguez-García I, Roszkowski L, Ruhland JB, Sanchez García E, Sánchez-Pastor T, Santorelli R, Seth S, Sinclair D, Skensved P, Smith B, Smith NJT, Sonley T, Stainforth R, Stringer M, Sur B, Vázquez-Jáuregui E, Viel S, Walding J, Waqar M, Ward M, Westerdale S, Willis J, and Zuñiga-Reyes A

Abstract

Dark matter with Planck-scale mass (≃10^{19}  GeV/c^{2}) arises in well-motivated theories and could be produced by several cosmological mechanisms. A search for multiscatter signals from supermassive dark matter was performed with a blind analysis of data collected over a 813 d live time with DEAP-3600, a 3.3 t single-phase liquid argon-based detector at SNOLAB. No candidate signals were observed, leading to the first direct detection constraints on Planck-scale mass dark matter. Leading limits constrain dark matter masses between 8.3×10^{6} and 1.2×10^{19}  GeV/c^{2}, and ^{40}Ar-scattering cross sections between 1.0×10^{-23} and 2.4×10^{-18}  cm^{2}. These results are interpreted as constraints on composite dark matter models with two different nucleon-to-nuclear cross section scalings.

Published
2022
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24. Pulse-shape discrimination against low-energy Ar-39 beta decays in liquid argon with 4.5 tonne-years of DEAP-3600 data.

Author

Adhikari P, Ajaj R, Alpízar-Venegas M, Amaudruz PA, Auty DJ, Batygov M, Beltran B, Benmansour H, Bina CE, Bonatt J, Bonivento W, Boulay MG, Broerman B, Bueno JF, Burghardt PM, Butcher A, Cadeddu M, Cai B, Cárdenas-Montes M, Cavuoti S, Chen M, Chen Y, Cleveland BT, Corning JM, Cranshaw D, Daugherty S, DelGobbo P, Dering K, DiGioseffo J, Di Stefano P, Doria L, Duncan FA, Dunford M, Ellingwood E, Erlandson A, Farahani SS, Fatemighomi N, Fiorillo G, Florian S, Flower T, Ford RJ, Gagnon R, Gallacher D, García Abia P, Garg S, Giampa P, Goeldi D, Golovko V, Gorel P, Graham K, Grant DR, Grobov A, Hallin AL, Hamstra M, Harvey PJ, Hearns C, Hugues T, Ilyasov A, Joy A, Jigmeddorj B, Jillings CJ, Kamaev O, Kaur G, Kemp A, Kochanek I, Kuźniak M, Lai M, Langrock S, Lehnert B, Leonhardt A, Levashko N, Li X, Lidgard J, Lindner T, Lissia M, Lock J, Longo G, Machulin I, McDonald AB, McElroy T, McGinn T, McLaughlin JB, Mehdiyev R, Mielnichuk C, Monroe J, Nadeau P, Nantais C, Ng C, Noble AJ, O'Dwyer E, Oliviéro G, Ouellet C, Pal S, Pasuthip P, Peeters SJM, Perry M, Pesudo V, Picciau E, Piro MC, Pollmann TR, Rand ET, Rethmeier C, Retière F, Rodríguez-García I, Roszkowski L, Ruhland JB, Sánchez-García E, Santorelli R, Sinclair D, Skensved P, Smith B, Smith NJT, Sonley T, Soukup J, Stainforth R, Stone C, Strickland V, Stringer M, Sur B, Tang J, Vázquez-Jáuregui E, Viel S, Walding J, Waqar M, Ward M, Westerdale S, Willis J, and Zuñiga-Reyes A

Abstract

The DEAP-3600 detector searches for the scintillation signal from dark matter particles scattering on a 3.3 tonne liquid argon target. The largest background comes from 39 Ar beta decays and is suppressed using pulse-shape discrimination (PSD). We use two types of PSD estimator: the prompt-fraction, which considers the fraction of the scintillation signal in a narrow and a wide time window around the event peak, and the log-likelihood-ratio, which compares the observed photon arrival times to a signal and a background model. We furthermore use two algorithms to determine the number of photons detected at a given time: (1) simply dividing the charge of each PMT pulse by the mean single-photoelectron charge, and (2) a likelihood analysis that considers the probability to detect a certain number of photons at a given time, based on a model for the scintillation pulse shape and for afterpulsing in the light detectors. The prompt-fraction performs approximately as well as the log-likelihood-ratio PSD algorithm if the photon detection times are not biased by detector effects. We explain this result using a model for the information carried by scintillation photons as a function of the time when they are detected., (© The Author(s) 2021.)

Published
2021
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25. First Results from the DEAP-3600 Dark Matter Search with Argon at SNOLAB.

Author

Amaudruz PA, Baldwin M, Batygov M, Beltran B, Bina CE, Bishop D, Bonatt J, Boorman G, Boulay MG, Broerman B, Bromwich T, Bueno JF, Burghardt PM, Butcher A, Cai B, Chan S, Chen M, Chouinard R, Cleveland BT, Cranshaw D, Dering K, DiGioseffo J, Dittmeier S, Duncan FA, Dunford M, Erlandson A, Fatemighomi N, Florian S, Flower A, Ford RJ, Gagnon R, Giampa P, Golovko VV, Gorel P, Gornea R, Grace E, Graham K, Gulyev E, Hakobyan R, Hall A, Hallin AL, Hamstra M, Harvey PJ, Hearns C, Jillings CJ, Kamaev O, Kemp A, Kuźniak M, Langrock S, La Zia F, Lehnert B, Lidgard JJ, Lim C, Lindner T, Linn Y, Liu S, Majewski P, Mathew R, McDonald AB, McElroy T, McGinn T, McLaughlin JB, Mead S, Mehdiyev R, Mielnichuk C, Monroe J, Muir A, Nadeau P, Nantais C, Ng C, Noble AJ, O'Dwyer E, Ohlmann C, Olchanski K, Olsen KS, Ouellet C, Pasuthip P, Peeters SJM, Pollmann TR, Rand ET, Rau W, Rethmeier C, Retière F, Seeburn N, Shaw B, Singhrao K, Skensved P, Smith B, Smith NJT, Sonley T, Soukup J, Stainforth R, Stone C, Strickland V, Sur B, Tang J, Taylor J, Veloce L, Vázquez-Jáuregui E, Walding J, Ward M, Westerdale S, Woolsey E, and Zielinski J

Abstract

This Letter reports the first results of a direct dark matter search with the DEAP-3600 single-phase liquid argon (LAr) detector. The experiment was performed 2 km underground at SNOLAB (Sudbury, Canada) utilizing a large target mass, with the LAr target contained in a spherical acrylic vessel of 3600 kg capacity. The LAr is viewed by an array of PMTs, which would register scintillation light produced by rare nuclear recoil signals induced by dark matter particle scattering. An analysis of 4.44 live days (fiducial exposure of 9.87 ton day) of data taken during the initial filling phase demonstrates the best electronic recoil rejection using pulse-shape discrimination in argon, with leakage <1.2×10^{-7} (90% C.L.) between 15 and 31  keV&#95;{ee}. No candidate signal events are observed, which results in the leading limit on weakly interacting massive particle (WIMP)-nucleon spin-independent cross section on argon, <1.2×10^{-44}  cm^{2} for a 100  GeV/c^{2} WIMP mass (90% C.L.).

Published
2018
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26. Independent measurement of the total active 8B solar neutrino flux using an array of 3He proportional counters at the Sudbury Neutrino Observatory.

Author

Aharmim B, Ahmed SN, Amsbaugh JF, Anthony AE, Banar J, Barros N, Beier EW, Bellerive A, Beltran B, Bergevin M, Biller SD, Boudjemline K, Boulay MG, Bowles TJ, Browne MC, Bullard TV, Burritt TH, Cai B, Chan YD, Chauhan D, Chen M, Cleveland BT, Cox-Mobrand GA, Currat CA, Dai X, Deng H, Detwiler J, DiMarco M, Doe PJ, Doucas G, Drouin PL, Duba CA, Duncan FA, Dunford M, Earle ED, Elliott SR, Evans HC, Ewan GT, Farine J, Fergani H, Fleurot F, Ford RJ, Formaggio JA, Fowler MM, Gagnon N, Germani JV, Goldschmidt A, Goon JT, Graham K, Guillian E, Habib S, Hahn RL, Hallin AL, Hallman ED, Hamian AA, Harper GC, Harvey PJ, Hazama R, Heeger KM, Heintzelman WJ, Heise J, Helmer RL, Henning R, Hime A, Howard C, Howe MA, Huang M, Jagam P, Jamieson B, Jelley NA, Keeter KJ, Klein JR, Kormos LL, Kos M, Krüger A, Kraus C, Krauss CB, Kutter T, Kyba CC, Lange R, Law J, Lawson IT, Lesko KT, Leslie JR, Loach JC, MacLellan R, Majerus S, Mak HB, Maneira J, Martin R, McBryde K, McCauley N, McDonald AB, McGee S, Mifflin C, Miller GG, Miller ML, Monreal B, Monroe J, Morissette B, Myers A, Nickel BG, Noble AJ, Oblath NS, O'Keeffe HM, Ollerhead RW, Gann GD, Oser SM, Ott RA, Peeters SJ, Poon AW, Prior G, Reitzner SD, Rielage K, Robertson BC, Robertson RG, Rollin E, Schwendener MH, Secrest JA, Seibert SR, Simard O, Simpson JJ, Sinclair L, Skensved P, Smith MW, Steiger TD, Stonehill LC, Tesić G, Thornewell PM, Tolich N, Tsui T, Tunnell CD, Van Wechel T, Van Berg R, VanDevender BA, Virtue CJ, Walker TJ, Wall BL, Waller D, Tseung HW, Wendland J, West N, Wilhelmy JB, Wilkerson JF, Wilson JR, Wouters JM, Wright A, Yeh M, Zhang F, and Zuber K

Abstract

The Sudbury Neutrino Observatory (SNO) used an array of 3He proportional counters to measure the rate of neutral-current interactions in heavy water and precisely determined the total active (nu&#95;x) 8B solar neutrino flux. This technique is independent of previous methods employed by SNO. The total flux is found to be 5.54&#95;-0.31;+0.33(stat)-0.34+0.36(syst)x10(6) cm(-2) s(-1), in agreement with previous measurements and standard solar models. A global analysis of solar and reactor neutrino results yields Deltam2=7.59&#95;-0.21;+0.19x10(-5) eV2 and theta=34.4&#95;-1.2;+1.3 degrees. The uncertainty on the mixing angle has been reduced from SNO's previous results.

Published
2008
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27. Measurement of the total active 8B solar neutrino flux at the Sudbury Neutrino Observatory with enhanced neutral current sensitivity.

Author

Ahmed SN, Anthony AE, Beier EW, Bellerive A, Biller SD, Boger J, Boulay MG, Bowler MG, Bowles TJ, Brice SJ, Bullard TV, Chan YD, Chen M, Chen X, Cleveland BT, Cox GA, Dai X, Dalnoki-Veress F, Doe PJ, Dosanjh RS, Doucas G, Dragowsky MR, Duba CA, Duncan FA, Dunford M, Dunmore JA, Earle ED, Elliott SR, Evans HC, Ewan GT, Farine J, Fergani H, Fleurot F, Formaggio JA, Fowler MM, Frame K, Fulsom BG, Gagnon N, Graham K, Grant DR, Hahn RL, Hall JC, Hallin AL, Hallman ED, Hamer AS, Handler WB, Hargrove CK, Harvey PJ, Hazama R, Heeger KM, Heintzelman WJ, Heise J, Helmer RL, Hemingway RJ, Hime A, Howe MA, Jagam P, Jelley NA, Klein JR, Kos MS, Krumins AV, Kutter T, Kyba CC, Labranche H, Lange R, Law J, Lawson IT, Lesko KT, Leslie JR, Levine I, Luoma S, MacLellan R, Majerus S, Mak HB, Maneira J, Marino AD, McCauley N, McDonald AB, McGee S, McGregor G, Mifflin C, Miknaitis KK, Miller GG, Moffat BA, Nally CW, Nickel BG, Noble AJ, Norman EB, Oblath NS, Okada CE, Ollerhead RW, Orrell JL, Oser SM, Ouellet C, Peeters SJ, Poon AW, Robertson BC, Robertson RG, Rollin E, Rosendahl SS, Rusu VL, Schwendener MH, Simard O, Simpson JJ, Sims CJ, Sinclair D, Skensved P, Smith MW, Starinsky N, Stokstad RG, Stonehill LC, Tafirout R, Takeuchi Y, Tesić G, Thomson M, Thorman M, Van Berg R, Van de Water RG, Virtue CJ, Wall BL, Waller D, Waltham CE, Tseung HW, Wark DL, West N, Wilhelmy JB, Wilkerson JF, Wilson JR, Wouters JM, Yeh M, and Zuber K

Abstract

The Sudbury Neutrino Observatory has precisely determined the total active (nu(x)) 8B solar neutrino flux without assumptions about the energy dependence of the nu(e) survival probability. The measurements were made with dissolved NaCl in heavy water to enhance the sensitivity and signature for neutral-current interactions. The flux is found to be 5.21 +/- 0.27(stat)+/-0.38(syst) x 10(6) cm(-2) s(-1), in agreement with previous measurements and standard solar models. A global analysis of these and other solar and reactor neutrino results yields Deltam(2)=7.1(+1.2)(-0.6) x 10(-5) eV(2) and theta=32.5(+2.4)(-2.3) degrees. Maximal mixing is rejected at the equivalent of 5.4 standard deviations.

Published
2004
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28. Constraints on nucleon decay via invisible modes from the Sudbury Neutrino Observatory.

Author

Ahmed SN, Anthony AE, Beier EW, Bellerive A, Biller SD, Boger J, Boulay MG, Bowler MG, Bowles TJ, Brice SJ, Bullard TV, Chan YD, Chen M, Chen X, Cleveland BT, Cox GA, Dai X, Dalnoki-Veress F, Doe PJ, Dosanjh RS, Doucas G, Dragowsky MR, Duba CA, Duncan FA, Dunford M, Dunmore JA, Earle ED, Elliott SR, Evans HC, Ewan GT, Farine J, Fergani H, Fleurot F, Formaggio JA, Fowler MM, Frame K, Frati W, Fulsom BG, Gagnon N, Graham K, Grant DR, Hahn RL, Hall JC, Hallin AL, Hallman ED, Hamer AS, Handler WB, Hargrove CK, Harvey PJ, Hazama R, Heeger KM, Heintzelman WJ, Heise J, Helmer RL, Hemingway RJ, Hime A, Howe MA, Jagam P, Jelley NA, Klein JR, Kos MS, Krumins AV, Kutter T, Kyba CC, Labranche H, Lange R, Law J, Lawson IT, Lesko KT, Leslie JR, Levine I, Luoma S, MacLellan R, Majerus S, Mak HB, Maneira J, Marino AD, McCauley N, McDonald AB, McGee S, McGregor G, Mifflin C, Miknaitis KK, Miller GG, Moffat BA, Nally CW, Neubauer MS, Nickel BG, Noble AJ, Norman EB, Oblath NS, Okada CE, Ollerhead RW, Orrell JL, Oser SM, Ouellet C, Peeters SJ, Poon AW, Robertson BC, Robertson RG, Rollin E, Rosendahl SS, Rusu VL, Schwendener MH, Simard O, Simpson JJ, Sims CJ, Sinclair D, Skensved P, Smith MW, Starinsky N, Stokstad RG, Stonehill LC, Tafirout R, Takeuchi Y, Tesić G, Thomson M, Thorman M, Van Berg R, Van de Water RG, Virtue CJ, Wall BL, Waller D, Waltham CE, Tseung HW, Wark DL, West N, Wilhelmy JB, Wilkerson JF, Wilson JR, Wittich P, Wouters JM, Yeh M, and Zuber K

Abstract

Data from the Sudbury Neutrino Observatory have been used to constrain the lifetime for nucleon decay to "invisible" modes, such as n-->3nu. The analysis was based on a search for gamma rays from the deexcitation of the residual nucleus that would result from the disappearance of either a proton or neutron from 16O. A limit of tau(inv)>2 x 10(29) yr is obtained at 90% confidence for either neutron- or proton-decay modes. This is about an order of magnitude more stringent than previous constraints on invisible proton-decay modes and 400 times more stringent than similar neutron modes.

Published
2004
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29. Measurement of day and night neutrino energy spectra at SNO and constraints on neutrino mixing parameters.

Author

Ahmad QR, Allen RC, Andersen TC, Anglin JD, Barton JC, Beier EW, Bercovitch M, Bigu J, Biller SD, Black RA, Blevis I, Boardman RJ, Boger J, Bonvin E, Boulay MG, Bowler MG, Bowles TJ, Brice SJ, Browne MC, Bullard TV, Bühler G, Cameron J, Chan YD, Chen HH, Chen M, Chen X, Cleveland BT, Clifford ET, Cowan JH, Cowen DF, Cox GA, Dai X, Dalnoki-Veress F, Davidson WF, Doe PJ, Doucas G, Dragowsky MR, Duba CA, Duncan FA, Dunford M, Dunmore JA, Earle ED, Elliott SR, Evans HC, Ewan GT, Farine J, Fergani H, Ferraris AP, Ford RJ, Formaggio JA, Fowler MM, Frame K, Frank ED, Frati W, Gagnon N, Germani JV, Gil S, Graham K, Grant DR, Hahn RL, Hallin AL, Hallman ED, Hamer AS, Hamian AA, Handler WB, Haq RU, Hargrove CK, Harvey PJ, Hazama R, Heeger KM, Heintzelman WJ, Heise J, Helmer RL, Hepburn JD, Heron H, Hewett J, Hime A, Howe M, Hykawy JG, Isaac MC, Jagam P, Jelley NA, Jillings C, Jonkmans G, Kazkaz K, Keener PT, Klein JR, Knox AB, Komar RJ, Kouzes R, Kutter T, Kyba CC, Law J, Lawson IT, Lay M, Lee HW, Lesko KT, Leslie JR, Levine I, Locke W, Luoma S, Lyon J, Majerus S, Mak HB, Maneira J, Manor J, Marino AD, McCauley N, McDonald AB, McDonald DS, McFarlane K, McGregor G, Meijer Drees R, Mifflin C, Miller GG, Milton G, Moffat BA, Moorhead M, Nally CW, Neubauer MS, Newcomer FM, Ng HS, Noble AJ, Norman EB, Novikov VM, O'Neill M, Okada CE, Ollerhead RW, Omori M, Orrell JL, Oser SM, Poon AW, Radcliffe TJ, Roberge A, Robertson BC, Robertson RG, Rosendahl SS, Rowley JK, Rusu VL, Saettler E, Schaffer KK, Schwendener MH, Schülke A, Seifert H, Shatkay M, Simpson JJ, Sims CJ, Sinclair D, Skensved P, Smith AR, Smith MW, Spreitzer T, Starinsky N, Steiger TD, Stokstad RG, Stonehill LC, Storey RS, Sur B, Tafirout R, Tagg N, Tanner NW, Taplin RK, Thorman M, Thornewell PM, Trent PT, Tserkovnyak YI, Van Berg R, Van de Water RG, Virtue CJ, Waltham CE, Wang JX, Wark DL, West N, Wilhelmy JB, Wilkerson JF, Wilson JR, Wittich P, Wouters JM, and Yeh M

Abstract

The Sudbury Neutrino Observatory (SNO) has measured day and night solar neutrino energy spectra and rates. For charged current events, assuming an undistorted 8B spectrum, the night minus day rate is 14.0%+/-6.3%(+1.5%)(-1.4%) of the average rate. If the total flux of active neutrinos is additionally constrained to have no asymmetry, the nu(e) asymmetry is found to be 7.0%+/-4.9%(+1.3%)(-1.2%). A global solar neutrino analysis in terms of matter-enhanced oscillations of two active flavors strongly favors the large mixing angle solution.

Published
2002
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30. Direct evidence for neutrino flavor transformation from neutral-current interactions in the Sudbury Neutrino Observatory.

Author

Ahmad QR, Allen RC, Andersen TC, D Anglin J, Barton JC, Beier EW, Bercovitch M, Bigu J, Biller SD, Black RA, Blevis I, Boardman RJ, Boger J, Bonvin E, Boulay MG, Bowler MG, Bowles TJ, Brice SJ, Browne MC, Bullard TV, Bühler G, Cameron J, Chan YD, Chen HH, Chen M, Chen X, Cleveland BT, Clifford ET, Cowan JH, Cowen DF, Cox GA, Dai X, Dalnoki-Veress F, Davidson WF, Doe PJ, Doucas G, Dragowsky MR, Duba CA, Duncan FA, Dunford M, Dunmore JA, Earle ED, Elliott SR, Evans HC, Ewan GT, Farine J, Fergani H, Ferraris AP, Ford RJ, Formaggio JA, Fowler MM, Frame K, Frank ED, Frati W, Gagnon N, Germani JV, Gil S, Graham K, Grant DR, Hahn RL, Hallin AL, Hallman ED, Hamer AS, Hamian AA, Handler WB, Haq RU, Hargrove CK, Harvey PJ, Hazama R, Heeger KM, Heintzelman WJ, Heise J, Helmer RL, Hepburn JD, Heron H, Hewett J, Hime A, Howe M, Hykawy JG, Isaac MC, Jagam P, Jelley NA, Jillings C, Jonkmans G, Kazkaz K, Keener PT, Klein JR, Knox AB, Komar RJ, Kouzes R, Kutter T, Kyba CC, Law J, Lawson IT, Lay M, Lee HW, Lesko KT, Leslie JR, Levine I, Locke W, Luoma S, Lyon J, Majerus S, Mak HB, Maneira J, Manor J, Marino AD, McCauley N, McDonald AB, McDonald DS, McFarlane K, McGregor G, Meijer Drees R, Mifflin C, Miller GG, Milton G, Moffat BA, Moorhead M, Nally CW, Neubauer MS, Newcomer FM, Ng HS, Noble AJ, Norman EB, Novikov VM, O'Neill M, Okada CE, Ollerhead RW, Omori M, Orrell JL, Oser SM, Poon AW, Radcliffe TJ, Roberge A, Robertson BC, Robertson RG, Rosendahl SS, Rowley JK, Rusu VL, Saettler E, Schaffer KK, Schwendener MH, Schülke A, Seifert H, Shatkay M, Simpson JJ, Sims CJ, Sinclair D, Skensved P, Smith AR, Smith MW, Spreitzer T, Starinsky N, Steiger TD, Stokstad RG, Stonehill LC, Storey RS, Sur B, Tafirout R, Tagg N, Tanner NW, Taplin RK, Thorman M, Thornewell PM, Trent PT, Tserkovnyak YI, Van Berg R, Van de Water RG, Virtue CJ, Waltham CE, Wang JX, Wark DL, West N, Wilhelmy JB, Wilkerson JF, Wilson JR, Wittich P, Wouters JM, and Yeh M

Abstract

Observations of neutral-current nu interactions on deuterium in the Sudbury Neutrino Observatory are reported. Using the neutral current (NC), elastic scattering, and charged current reactions and assuming the standard 8B shape, the nu(e) component of the 8B solar flux is phis(e) = 1.76(+0.05)(-0.05)(stat)(+0.09)(-0.09)(syst) x 10(6) cm(-2) s(-1) for a kinetic energy threshold of 5 MeV. The non-nu(e) component is phi(mu)(tau) = 3.41(+0.45)(-0.45)(stat)(+0.48)(-0.45)(syst) x 10(6) cm(-2) s(-1), 5.3sigma greater than zero, providing strong evidence for solar nu(e) flavor transformation. The total flux measured with the NC reaction is phi(NC) = 5.09(+0.44)(-0.43)(stat)(+0.46)(-0.43)(syst) x 10(6) cm(-2) s(-1), consistent with solar models.

Published
2002
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31. Measurement of the rate of nu(e) + d --> p + p + e(-) interactions produced by (8)B solar neutrinos at the Sudbury Neutrino Observatory.

Author

Ahmad QR, Allen RC, Andersen TC, Anglin JD, Bühler G, Barton JC, Beier EW, Bercovitch M, Bigu J, Biller S, Black RA, Blevis I, Boardman RJ, Boger J, Bonvin E, Boulay MG, Bowler MG, Bowles TJ, Brice SJ, Browne MC, Bullard TV, Burritt TH, Cameron K, Cameron J, Chan YD, Chen M, Chen HH, Chen X, Chon MC, Cleveland BT, Clifford ET, Cowan JH, Cowen DF, Cox GA, Dai Y, Dai X, Dalnoki-Veress F, Davidson WF, Doe PJ, Doucas G, Dragowsky MR, Duba CA, Duncan FA, Dunmore J, Earle ED, Elliott SR, Evans HC, Ewan GT, Farine J, Fergani H, Ferraris AP, Ford RJ, Fowler MM, Frame K, Frank ED, Frati W, Germani JV, Gil S, Goldschmidt A, Grant DR, Hahn RL, Hallin AL, Hallman ED, Hamer A, Hamian AA, Haq RU, Hargrove CK, Harvey PJ, Hazama R, Heaton R, Heeger KM, Heintzelman WJ, Heise J, Helmer RL, Hepburn JD, Heron H, Hewett J, Hime A, Howe M, Hykawy JG, Isaac MC, Jagam P, Jelley NA, Jillings C, Jonkmans G, Karn J, Keener PT, Kirch K, Klein JR, Knox AB, Komar RJ, Kouzes R, Kutter T, Kyba CC, Law J, Lawson IT, Lay M, Lee HW, Lesko KT, Leslie JR, Levine I, Locke W, Lowry MM, Luoma S, Lyon J, Majerus S, Mak HB, Marino AD, McCauley N, McDonald AB, McDonald DS, McFarlane K, McGregor G, McLatchie W, Meijer Drees R, Mes H, Mifflin C, Miller GG, Milton G, Moffat BA, Moorhead M, Nally CW, Neubauer MS, Newcomer FM, Ng HS, Noble AJ, Norman EB, Novikov VM, O'Neill M, Okada CE, Ollerhead RW, Omori M, Orrell JL, Oser SM, Poon AW, Radcliffe TJ, Roberge A, Robertson BC, Robertson RG, Rowley JK, Rusu VL, Saettler E, Schaffer KK, Schuelke A, Schwendener MH, Seifert H, Shatkay M, Simpson JJ, Sinclair D, Skensved P, Smith AR, Smith MW, Starinsky N, Steiger TD, Stokstad RG, Storey RS, Sur B, Tafirout R, Tagg N, Tanner NW, Taplin RK, Thorman M, Thornewell P, Trent PT, Tserkovnyak YI, Van Berg R, Van de Water RG, Virtue CJ, Waltham CE, Wang JX, Wark DL, West N, Wilhelmy JB, Wilkerson JF, Wilson J, Wittich P, Wouters JM, and Yeh M

Abstract

Solar neutrinos from (8)B decay have been detected at the Sudbury Neutrino Observatory via the charged current (CC) reaction on deuterium and the elastic scattering (ES) of electrons. The flux of nu(e)'s is measured by the CC reaction rate to be straight phi(CC)(nu(e)) = 1.75 +/- 0.07(stat)(+0.12)(-0.11)(syst) +/- 0.05(theor) x 10(6) cm(-2) s(-1). Comparison of straight phi(CC)(nu(e)) to the Super-Kamiokande Collaboration's precision value of the flux inferred from the ES reaction yields a 3.3 sigma difference, assuming the systematic uncertainties are normally distributed, providing evidence of an active non- nu(e) component in the solar flux. The total flux of active 8B neutrinos is determined to be 5.44+/-0.99 x 10(6) cm(-2) s(-1).

Published
2001
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32. The Russian-American gallium experiment (SAGE) Cr Neutrino source measurement.

Author

Abdurashitov JN, Gavrin VN, Girin SV, Gorbachev VV, Ibragimova TV, Kalikhov AV, Khairnasov NG, Knodel TV, Kornoukhov VN, Mirmov IN, Shikhin AA, Veretenkin EP, Vermul VM, Yants VE, Zatsepin GT, Bowles TJ, Nico JS, Teasdale WA, Wark DL, Cherry ML, Karaulov VN, Levitin VL, Maev VI VI, Nazarenko PI, Shkol'nik VS, Skorikov NV, Cleveland BT, Daily T, Davis R Jr, Lande K, Lee CK, Wildenhain PW, Khomyakov YS, Zvonarev AV, Elliott SR, and Wilkerson JF

Published
1996
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33. Status of the Soviet-American Gallium Experiment.

Author

Anosov OL, Bowles TJ, Cherry ML, Cleveland BT, Davis R Jr, Elliott SR, Faizov EL, Gavrin VN, Kalikhov AV, Knodel TV, Knyshenko II, Kornoukhov VN, Kouzes RT, Lande K, Miromov IN, Nico JS, O'Brien HA, Ostrinsky AV, Pshukov AM, Shikhin AA, Timofeyev PV, Veretenkin EP, Vermul VM, Wark DL, Wilkerson JF, and Zatsepin GT

Published
1993
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34. Search for neutrinos from the Sun using the reaction 71Ga( nu e,e-)71Ge.

Author

Abazov AI, Anosov OL, Faizov EL, Gavrin VN, Kalikhov AV, Knodel TV, Knyshenko II II, Kornoukhov VN, Mezentseva SA, Mirmov IN, Ostrinsky AV, Pshukov AM, Revzin NE, Shikhin AA, Timofeyev PV, Veretenkin EP, Vermul VM, Zatsepin GT, Bowles TJ, Cleveland BT, Elliott SR, O'Brien HA, Wark DL, Wilkerson JF, Davis R Jr, Lande K, Cherry ML, and Kouzes RT

Published
1991
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