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

Author

C. E. Okada, Ilan Levine, David A. Sinclair, D. Chauhan, J. Wendland, J. F. Wilkerson, B. Beltran, F. B. Descamps, Jocelyn Monroe, M. H. Schwendener, N. Gagnon, M. Jerkins, T. Sonley, F. Zhang, N. S. Oblath, G. D. Orebi Gann, H. Deng, B. Aharmim, J. R. Leslie, L. C. Stonehill, R. W. Ollerhead, J. Law, A. L. Hallin, B. T. Cleveland, B. C. Robertson, E. Blucher, Bei Cai, Ryuta Hazama, G. Doucas, K. Boudjemline, N. Tolich, M. Huang, H. Wan Chan Tseung, S. Habib, S. Majerus, Yuen-Dat Chan, K. Graham, T. Kutter, T. J. Winchester, Alain Bellerive, D. L. Wark, M. L. Miller, J. Heise, S. M. Oser, M. Bergevin, L. L. Kormos, R. D. Martin, Andrew Hime, N. McCauley, P. Jagam, S. R. Elliott, G. T. Ewan, C. Kraus, A. Krüger, Keith Rielage, R. G. H. Robertson, S. D. Reitzner, S. N. Ahmed, M. Kos, J. C. Loach, O. Simard, R. Van Berg, P. L. Drouin, K. Gilje, R. L. Hahn, I. Lawson, R. J. Ford, Monica Dunford, C. J. Virtue, E. W. Beier, A. J. Noble, J. Maneira, A. W. P. Poon, J. Caravaca, F. Fleurot, B. L. Wall, A. E. Anthony, Christopher C. M. Kyba, P. J. Doe, G. Prior, N. West, W. J. Heintzelman, Hal Evans, S. J. M. Peeters, C. Howard, J. Farine, H. M. O'Keeffe, K. T. Lesko, S. D. Biller, R. A. Ott, Bernie G. Nickel, P. J. Harvey, Jochen Klein, K. J. Keeter, E. Guillian, H. B. Mak, Minfang Yeh, G. Tešić, N. A. Jelley, S. McGee, J. Tm. Goon, N. Barros, A. B. McDonald, E. D. Hallman, R. MacLellan, T. Tsui, S. R. Seibert, Min Chen, C. B. Krauss, B. A. VanDevender, P. Skensved, D. Waller, B. Jamieson, R. Bonventre, James R. Wilson, B. J. Land, X. Dai, J. A. Secrest, J. A. Detwiler, G. A. Cox, R. Lange, Benjamin Monreal, A. Mastbaum, H. Fergani, R. L. Helmer, Kai Zuber, A. Wright, M. G. Boulay, A. LaTorre, E. J. Callaghan, K. Labe, and Joseph A. Formaggio

Subjects
Physics, Standard solar model, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Solar neutrino, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Supernova, 0103 physical sciences, High Energy Physics::Experiment, Nuclear Experiment (nucl-ex), Neutrino, 010306 general physics, Nuclear Experiment
Abstract

A search has been performed for neutrinos from two sources, the $hep$ reaction in the solar $pp$ fusion chain and the $��_e$ 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 $��_{hep} < 30\times10^{3}~\mathrm{cm}^{-2}~\mathrm{s}^{-1}$ [90% credible interval (CI)]. No events are observed in the DSNB search region, and we set an improved upper bound on the $��_e$ component of the DSNB flux of $��^\mathrm{DSNB}_{��_e} < 19~\textrm{cm}^{-2}~\textrm{s}^{-1}$ (90% CI) in the energy range $22.9 < E_��< 36.9$~MeV., 11 pages, 6 figures

Published
2020

2. The Benefit of Fentanyl in Effective Sedation and Quality of Upper Endoscopy: A Double-Blinded Randomized Trial of Fentanyl Added to Midazolam Versus Midazolam Alone for Sedation

Author

Subhas C. Ganguli, S. Jalali, R Spaziani, Keith Tsoi, David Morgan, H Fergani, and Khurram J. Khan

Subjects
Sedation, Placebo, law.invention, Fentanyl, 03 medical and health sciences, 0302 clinical medicine, Randomized controlled trial, law, Medicine, Retching, medicine.diagnostic_test, business.industry, Endoscopy, Original Articles, Quality, Clinical trial, 030220 oncology & carcinogenesis, Anesthesia, Midazolam, 030211 gastroenterology & hepatology, medicine.symptom, business, medicine.drug
Abstract

Aims Our goals were to compare the effect of adding fentanyl to midazolam in a double-blinded, randomized, placebo-controlled trial and determine if fentanyl enhances sedation, increases adverse events or effects time of the procedure or discharge. Methods Patients 18 to 65 years scheduled for outpatient upper endoscopy were eligible for the study. Patients were randomized to receive either 100 mcg/2 mL of Fentanyl or 2 mL of placebo IV with a double-blinded protocol. All patients received 2 mg of intravenous midazolam initially. Additional midazolam could be given to achieve adequate sedation. Results There were 68 patients randomized to the Fentanyl group and 69 patients to the placebo group. The mean dose of midazolam was 4.0 mg for the Fentanyl group and 5.2 mg for placebo group (P=0.003). Both endoscopist and nurse independently rated sedation to be better in the fentanyl group (P=0001). The patient did not perceive any difference in sedation (P=0.4). Procedure time was significantly shorter in the Fentanyl group (8.5 versus 11.1 minutes, P=0.001), with no difference in the discharge time. There was significantly less retching observed in patients in the fentanyl group (P

Published
2018
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3. A233 BASELINE BOWEL ROUTINE AND OTHER PREDICTORS OF BOWEL PREPARATION IN PATIENTS UNDERGOING OUT-PATIENT COLONOSCOPY; RESULTS FROM A PROSPECTIVE SINGLE-CENTRE STUDY

Author

A Nehvi, M Khan, Khalid S. Khan, David Morgan, Subhas C. Ganguli, R Spaziani, David Armstrong, S. Jalali, Kelvin K.F. Tsoi, and H Fergani

Subjects
medicine.medical_specialty, Single centre, medicine.diagnostic_test, business.industry, digestive, oral, and skin physiology, Bowel preparation, medicine, Colonoscopy, In patient, Posters Of Distinction, business, Baseline (configuration management), Surgery
Abstract

BACKGROUND: Bowel preparation is essential as a quality measure of colonoscopy. Many studies have reported factors associate with a good bowel preparation but few have evaluated the effect of baseline bowel habit as a predictor. AIMS: We aimed to identify factors associated with a good bowel preparation. Specifically, we wanted to determine if baseline bowel habit predicted response to bowel preparation and how accurate patient perception of their bowel preparation was compared to a standard bowel prep score. METHODS: Prospective data was collected from out-patients undergoing colonoscopy in the form of a survey in the waiting room of the endoscopy unit. Data included baseline patient and endoscopy factors, and was compared to endoscopist reported Ottawa Bowel Preparation Score (OBPS) to look for correlation in a statistical analysis. RESULTS: Data were available for 243 patients; mean age 57 years, 46% male, 51% had more than a high school education. PEG-Lyte solution (4L) was used for bowel preparation by 48 (19.8%) and sodium picosulfate by 190 (80.2%). The mean OBPS was 3.48 +/- 2.47 SD. The baseline Bristol Stool Form Score (BSFS) was 1–2 in 13%, 3–5 in 74%, and 6–7 in 13% of patients, but BSFS did not predict a better OBPS (p=0.82). The mean times from the patients’ last fluids and last solids food to colonoscopy was 5.47 +/- 5.0 and 27.8 +/- 4.8 hours respectively, but neither was a significant predictor of better bowel prep. More procedures were in the afternoon (78%) but there was no difference in the OBPS in the morning and afternoon (Mann-Whitney test, p=0.47). Self-assessment of the quality of bowel preparation was not correlated with OBPS (Spearman rho 0.03, p=0.63), but a patients’ level of concern with not having a clean enough preparation was correlated with a worse OBPS (Spearman rho -0.175, p=0.012). The only significant predictor in a univariate analysis was bowel preparation type with sodium picosulfate being significantly better (Mann Whitney test, p

Published
2019
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4. Measurement of radium concentration in water with Mn-coated beads at the Sudbury Neutrino Observatory

Author

T.C. Andersen, I. Blevis, J. Boger, E. Bonvin, M. Chen, B.T. Cleveland, X. Dai, F. Dalnoki-Veress, G. Doucas, J. Farine, H. Fergani, A.P. Ferraris, M.M. Fowler, R.L. Hahn, E.D. Hallman, C.K. Hargrove, P. Jagam, N.A. Jelley, A.B. Knox, H.W. Lee, I. Levine, S. Majerus, K. McFarlane, C. Mifflin, G.G. Miller, A.J. Noble, P. Palmer, J.K. Rowley, M. Shatkay, J.J. Simpson, D. Sinclair, J.-X. Wang, J.B. Wilhelmy, and M. Yeh

Subjects
Detection limit, Physics, Heavy water, Nuclear and High Energy Physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Solar neutrino, Counting efficiency, Analytical chemistry, FOS: Physical sciences, chemistry.chemical_element, 01 natural sciences, Ion, Radium, chemistry.chemical_compound, Adsorption, chemistry, 0103 physical sciences, Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Experiment, Instrumentation
Abstract

We describe a method to measure the concentration of 224Ra and 226Ra in the heavy water target used to detect solar neutrinos at the Sudbury Neutrino Observatory and in the surrounding light water shielding. A water volume of (50-400) m^3 from the detector is passed through columns which contain beads coated with a compound of manganese oxide onto which the Ra dissolved in the water is adsorbed. The columns are removed, dried, and mounted below an electrostatic chamber into which the Rn from the decay of trapped Ra is continuously flowed by a stream of nitrogen gas. The subsequent decay of Rn gives charged Po ions which are swept by the electric field onto a solid-state alpha counter. The content of Ra in the water is inferred from the measured decay rates of 212Po, 214Po, 216Po, and 218Po. The Ra extraction efficiency is >95%, the counting efficiency is 24% for 214Po and 6% for 216Po, and the method can detect a few atoms of 224Ra per m^3 and a few tens of thousands of atoms of 226Ra per m^3. Converted to equivalent equilibrium values of the topmost elements of the natural radioactive chains, the detection limit in a single assay is a few times 10^(-16) g Th or U/cm^3. The results of some typical assays are presented and the contributions to the systematic error are discussed., 25 pages, 8 figures. V2 shortened to 17 pages, 5 figures

Published
2016
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5. Neutral current and day night measurements from the pure D2O phase of SNO

Author

B. C. Robertson, J. R. Leslie, M. Dunford, Eric B. Norman, J. B. Wilhelmy, T. Kutter, J. Manor, J. Farine, S. D. Biller, C. W. Nally, T. V. Bullard, A. S. Hamer, D. R. Grant, Guthrie Miller, S. J. Brice, James R. Wilson, E. W. Beier, P. J. Harvey, J. Cameron, C. E. Okada, J. F. Wilkerson, E. D. Hallman, X. Chen, W. J. Heintzelman, S. R. Elliott, R. G. Stokstad, David A. Sinclair, J. A. Formaggio, P. Jagam, Reda Tafirout, Christopher C. M. Kyba, M. W. Smith, C. J. Virtue, Ilan Levine, H. B. Mak, R. G. Van de Water, N. Starinsky, G. Doucas, P. Skensved, G. T. Ewan, K. K. Schaffer, G. A. Cox, K. Kazkaz, M. M. Fowler, F. Dalnoki-Veress, M. G. Bowler, C. K. Hargrove, K. Graham, S. M. Oser, P. T. Keener, S. S.E. Rosendahl, S. Majerus, John L. Orrell, Hal Evans, W. Frati, S. Luoma, B. T. Cleveland, W. B. Handler, D. L. Wark, K. T. Lesko, N. Tagg, E. D. Earle, N. Gagnon, Y.D. Chan, K. M. Heeger, A. Hime, Mark Guy Boulay, X. Dai, J. J. Simpson, R. L. Hahn, R. Hazama, Minfang Yeh, J. A. Dunmore, N. A. Jelley, K. Frame, A. L. Hallin, M. Howe, J. M. Wouters, Peter Wittich, A. B. McDonald, N. McCauley, A. D. Marino, R. Van Berg, H. Fergani, M. L. Chen, I. Lawson, A. J. Noble, Jochen Klein, V. L. Rusu, J. Maneira, A. W. P. Poon, F. A. Duncan, R. G. H. Robertson, M. R. Dragowsky, T. Spreitzer, T.J. Bowles, G. McGregor, Chris Waltham, L. C. Stonehill, R. L. Helmer, M. H. Schwendener, J. Law, C. J. Sims, J. Heise, C. A. Duba, N. West, and P. J. Doe

Subjects
Physics, Elastic scattering, Nuclear and High Energy Physics, Sudbury Neutrino Observatory, Solar neutrino, Atomic and Molecular Physics, and Optics, Massless particle, Nuclear physics, Neutrino detector, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Neutrino, Nuclear Experiment, Charged current, Lepton
Abstract

The Sudbury Neutrino Observatory is a 1000 T D 2 O Cerenkov detector that is sensitive to 8 B solar neutrinos. The energy, radius, and direction with respect to the sun is measured for each neutrino event; these distributions are used to separately determine the rates of the charged current, neutral current and electron scattering reactions of neutrinos on deuterium. Assuming an undistorted 8 B spectrum, the ν e component of the 8 B solar flux is φ e = 1.76 +0.05 −0.05 (stat.) +0.09 −0.09 (syst.) × 10 6 cm −2 s −1 based on events with a measured kinetic enegy above 5 MeV. The non- ν e component is φ μτ = 3.41 +0.45 −0.45 (stat.) +0.48 −0.45 (syst.) × 10 6 cm −2 s −1 , 5.3 σ greater than zero, providing strong evidence for solar ν e flavor transformation. The total flux measured with the NC reaction is φ NC = 5.09 +0.044 −0.43 (stat.) +0.46 −0.43 (syst.) × 10 6 cm −2 s −1 , consistent with solar models. 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 ν e asymmetry is found to be 7.0% ± 4.9% +1.3 −1.2 %. A global solar neutrino analysis is terms of matter-enhanced oscillations of two active flavors strongly favors the Large Mixing Angle (LMA) solution.

Published
2016
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6. Constraints on nucleon decay via invisible modes from the Sudbury Neutrino Observatory

Author

X. Chen, H. Wan Chan Tseung, H. Labranche, D. L. Wark, F. Dalnoki-Veress, A. D. Marino, B. C. Robertson, N. McCauley, R. L. Helmer, G. Doucas, R. Van Berg, R. G. H. Robertson, J. B. Wilhelmy, T. Kutter, M. G. Bowler, I. Levine, M. L. Chen, Monica Dunford, S. S.E. Rosendahl, Chris Waltham, C. J. Virtue, S. J. Brice, A. W. P. Poon, J. A. Dunmore, R. L. Hahn, R. W. Ollerhead, C. W. Nally, G. McGregor, P. Jagam, K.K.S. Miknaitis, J. M. Wouters, S. Majerus, P. Skensved, X. Dai, J. F. Wilkerson, R. G. Van de Water, Joshua R. Klein, N. Gagnon, Reda Tafirout, N. Starinsky, Darren Grant, Alain Bellerive, R. S. Dosanjh, R. Lange, Mark Neubauer, W. Frati, S. N. Ahmed, R. Hazama, E. D. Earle, E. Rollin, W. B. Handler, H. B. Mak, T. J. Bowles, Andrew Hime, J. R. Wilson, Guthrie Miller, M. W.E. Smith, F. A. Duncan, M. A. Howe, A. B. McDonald, Christopher C. M. Kyba, R. MacLellan, M. A. Thomson, J. Heise, S. D. Biller, J. R. Leslie, B. A. Moffat, Bernie G. Nickel, J. Boger, F. Fleurot, M. H. Schwendener, B. T. Cleveland, Malcolm M. Fowler, N. S. Oblath, A. E. Anthony, N. West, A. V. Krumins, C. A. Duba, S. Luoma, Joseph A. Formaggio, C. Ouellet, Minfang Yeh, C. E. Okada, P. J. Harvey, W. J. Heintzelman, S. R. Elliott, O. Simard, David A. Sinclair, G. T. Ewan, I. T. Lawson, G. Tešić, A. L. Hallin, C. Mifflin, S. J. M. Peeters, N. A. Jelley, M. Thorman, D. Waller, V. L. Rusu, J. C. Hall, J. Law, M. R. Dragowsky, G. A. Cox, K. T. Lesko, L. C. Stonehill, J. Farine, C. J. Sims, C. K. Hargrove, A. J. Noble, T. V. Bullard, R. J. Hemingway, Kai Zuber, H. Fergani, J. Maneira, M. Kos, A. S. Hamer, Hal Evans, E. W. Beier, S. McGee, R. G. Stokstad, B. L. Wall, Peter Wittich, Eric B. Norman, E. D. Hallman, P. J. Doe, Y. Takeuchi, J. J. Simpson, Yuen-Dat Chan, K. Graham, S. M. Oser, M.G. Boulay, B. G. Fulsom, K. Frame, K. M. Heeger, and John L. Orrell

Subjects
Physics, Sudbury Neutrino Observatory, Particle physics, Proton, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Nuclear Theory, Gamma ray, FOS: Physical sciences, General Physics and Astronomy, Elementary particle, 01 natural sciences, High Energy Physics - Experiment, Nuclear physics, Baryon, High Energy Physics - Experiment (hep-ex), Particle decay, 0103 physical sciences, Neutron, High Energy Physics::Experiment, 010306 general physics, Nucleon, Nuclear Experiment
Abstract

Data from the Sudbury Neutrino Observatory have been used to constrain the lifetime for nucleon decay to ``invisible'' modes, such as n -> 3 nu. The analysis was based on a search for gamma-rays from the de-excitation of the residual nucleus that would result from the disappearance of either a proton or neutron from O16. A limit of tau_inv > 2 x 10^{29} years 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., Update includes missing efficiency factor (limits change by factor of 2) Submitted to Physical Review Letters

Published
2016
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7. SEARCHES FOR HIGH-FREQUENCY VARIATIONS IN THE B-8 SOLAR NEUTRINO FLUX AT THE SUDBURY NEUTRINO OBSERVATORY

Author

E. D. Hallman, G. Prior, Benjamin Monreal, E. D. Earle, P. J. Doe, S. J. M. Peeters, K. J. Keeter, T. Tsui, F. A. Duncan, P. Skensved, M. DiMarco, K. Boudjemline, Yuen-Dat Chan, J. M. Wouters, J. Heise, S. Habib, K. Graham, X. Dai, S. M. Oser, J. A. Detwiler, Keith Rielage, H. Wan Chan Tseung, M. L. Miller, A. B. McDonald, R. D. Martin, Andrew Hime, I. Levine, Jocelyn Monroe, Alain Bellerive, D. L. Wark, R. J. Ford, T. J. Sonley, R. L. Hahn, H. Fergani, R. G. H. Robertson, M. H. Schwendener, R. MacLellan, Monica Dunford, J. Maneira, B. Beltran, Mark Guy Boulay, Bei Cai, David A. Sinclair, C. A. Duba, F. Zhang, J. Law, D. Chauhan, Peter Watson, B. Jamieson, A. W. P. Poon, Christopher C. M. Kyba, P.-L. Drouin, N. Tolich, C. B. Krauss, N. S. Oblath, B. Aharmim, T.H. Burritt, Kai Zuber, C. D. Tunnell, A. L. Hallin, R. L. Helmer, B. Morissette, J. A. Secrest, I. T. Lawson, C. Kraus, B. T. Cleveland, S. R. Seibert, D. Waller, G. A. Cox, R. A. Ott, N. West, W. J. Heintzelman, K. T. Lesko, J. R. Wilson, M. Kos, A. Wright, O. Simard, E. W. Beier, B.A. VanDevender, L. C. Stonehill, C. Howard, J. Farine, A. J. Noble, C. J. Virtue, B. C. Robertson, G. Doucas, E. Guillian, T. Kutter, N. Barros, Joseph A. Formaggio, Minfang Yeh, J. C. Loach, N. A. Jelley, Hal Evans, S. D. Reitzner, S. N. Ahmed, Joshua R. Klein, M. Bergevin, N. McCauley, R. Van Berg, M. L. Chen, S. Majerus, L. L. Kormos, G. T. Ewan, N. Gagnon, R. Hazama, G. D. Orebi Gann, H. Deng, B. L. Wall, H. M. O'Keeffe, H. B. Mak, S. McGee, S. D. Biller, Bernie G. Nickel, P. J. Harvey, J. F. Wilkerson, Steven Elliott, M. A. Howe, M. Huang, G. Tešić, J. R. Leslie, F. Fleurot, A. E. Anthony, and J. Tm. Goon

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Solar neutrino, FOS: Physical sciences, Astrophysics, 01 natural sciences, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Nuclear Experiment (nucl-ex), 010303 astronomy & astrophysics, Nuclear Experiment, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Sudbury Neutrino Observatory, Solar observatory, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Solar neutrino problem, Neutrino detector, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Physics::Space Physics, Measurements of neutrino speed, Neutrino
Abstract

We have performed three searches for high-frequency signals in the solar neutrino flux measured by the Sudbury Neutrino Observatory (SNO), motivated by the possibility that solar $g$-mode oscillations could affect the production or propagation of solar $^8$B neutrinos. The first search looked for any significant peak in the frequency range 1/day to 144/day, with a sensitivity to sinusoidal signals with amplitudes of 12% or greater. The second search focused on regions in which $g$-mode signals have been claimed by experiments aboard the SoHO satellite, and was sensitive to signals with amplitudes of 10% or greater. The third search looked for extra power across the entire frequency band. No statistically significant signal was detected in any of the three searches., 37 pages, 17 figures, submitted to ApJ

Published
2016
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8. A235 EXPLORING PATIENT FACTORS FOR CANCELLED OR MISSED APPOINTMENTS TO AN URGENT GASTROENTEROLOGY OUTPATIENT CLINIC

Author

Khurram J. Khan, R Spaziani, David Morgan, H Fergani, Subhas C. Ganguli, W Kabir, S. Jalali, and Kelvin K.F. Tsoi

Subjects
medicine.medical_specialty, Abdominal pain, Lower gastrointestinal bleeding, Anemia, business.industry, General surgery, medicine.disease, Inflammatory bowel disease, Paper Sessions, Patient referral, medicine, Outpatient clinic, Upper gastrointestinal bleeding, medicine.symptom, business, Patient factors
Abstract

BACKGROUND: The Canadian Association of Gastroenterology reports that wait times to see a gastroenterologist are too long, even for urgent problems. Cancellations and no-shows compound this problem and lead to poor services utilization. A weekly urgent GI clinic started at St Joseph’s Healthcare Hamilton in March 2014 to improve timely access for patients. The clinic accepted referrals from the emergency room (ER) and urgent care with a capacity of 6 patients per week booked within 3 weeks of referral. The cancellation and absence rate from the clinic was 25% in the first 6 months despite patients receiving mail and phone reminder. Studies in no-show predictors focus on primary care, pediatric population and routine outpatient appointments. Published studies on absence rate in urgent clinic settings are very limited. AIMS: The present study explores patient factors for the high absence rate at our urgent GI clinic. METHODS: Retrospective review of patients booked to the urgent GI clinic between March and September 2014 that were absent at their appointment. The patient demographics, reasons for referrals, duration of symptoms were reviewed from the chart. The patients were contacted to explain why they missed their appointment and were offered to be rebooked. RESULTS: Between March and October 2014, 37 patients (25%) were absent for their appointment to the urgent GI clinic. The average age of patients was 51 years, and 43% were females. The mean duration of symptoms was 28.2 weeks, but 56% of patients had more acute symptoms for 1 week or less when presenting to ER or urgent care. The reasons for referrals included lower GI bleeding (24%), upper GI bleeding (22%), abdominal pain (16%), dysphagia (8%), anemia (5%) and inflammatory bowel disease (5%). Several attempts were made to contact patients, and 22/37 (59%) were reached. Of the 22 patients, 10 elected to cancel without rebooking, 3 were seen as inpatients, and 3 were seen by another outpatient gastroenterologist. Only 6/22 (27%) were rebooked to another urgent clinic appointment. CONCLUSIONS: The urgent GI clinic is a useful means for seeing patients with subacute GI illness but has an unacceptably high rate of missed appointments. Of the patients we contacted, only 27% were rebooked back to the urgent clinic. Almost half elected not to rebook suggesting that an urgent referral may not have been appropriate. On the other hand, 3 patients were admitted, suggesting that outpatient management may not have been suitable either, and 3 patients decided to follow up with their established gastroenterologist. The urgent GI clinic now screens all referrals for appropriateness, and does not see patients seen within the past year by another gastroenterologist. Follow-up data will hopefully demonstrate reduction in absence rate with this new strategy. FUNDING AGENCIES: None

Published
2018
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9. A236 UTILIZATION OF AN URGENT GASTROENTEROLOGY CLINIC FOR PATIENTS SEEN IN THE EMERGENCY ROOM OR URGENT CARE CENTRE

Author

Kelvin K.F. Tsoi, Subhas C. Ganguli, Khurram J. Khan, W Kabir, R Spaziani, S. Jalali, H Fergani, and David Morgan

Subjects
Waiting time, Patient referral, business.industry, medicine, Upper gastrointestinal bleeding, Medical emergency, medicine.disease, business, Gastroenterology clinic, Paper Sessions
Abstract

BACKGROUND: The Canadian Association of Gastroenterology reports that wait times to see a gastroenterologist are too long, even for urgent problems. To improve timely access for patients, a dedicated urgent GI clinic started at St Joseph’s Healthcare Hamilton in March 2014. The clinic accepted referrals from the emergency room (ER) and urgent care clinic with a capacity of 6 patients per week booked within 3 weeks of referral. Suggested referral criteria included a) subacute GI bleeding b) progressive dysphagia c) suspected diagnosis of IBD based on imaging/results and other reasons including liver diseases. AIMS: To review the utility of the clinic, appropriateness of referrals, and utilization of endoscopy resources to guide any necessary changes to the clinic. METHODS: Retrospective review of all cases that were seen in the urgent GI clinic to identify demographic factors, reasons for referrals, duration of symptoms, whether they had previously seen a gastroenterologist, utilization of endoscopy resources and requirement for ongoing follow up. RESULTS: Between March and October 2014, 119 patients were seen in the urgent GI clinic and 118 were reviewed. An average of 4.5 patients was seen per clinic out of 6 allocated spots giving a missed appointment rate of 25%. The average age of the patient was 52.9 years, and 57% were females. The mean duration of symptoms was 23.4 weeks, but 59% of patients had more acute symptoms for 1 week or less when presenting to ER or urgent care. The most common reasons for referrals included lower GI bleeding (31%), abdominal pain (25%), upper GI bleeding (13%), anemia (5%), and dysphagia (3%). Of the 119 patients, 42% had previously seen a gastroenterologist, and 46% had recently visited the ER or urgent care. A high proportion (71%) was booked for endoscopic tests after the consultation, and 52% were booked for a follow-up appointment. CONCLUSIONS: The urgent clinic provides a useful mechanism to see subacute GI illnesses in a timely fashion. However, further optimization is needed to reduce incidence of missed appointments, seeing patients already under care of a gastroenterologist, and referrals for chronic GI illness. There are challenges in high endoscopy utilization and clinic follow-up associated with this strategy. Longer studies may help illustrate further benefits of healthcare utilization by examining reduction in recurrent visits to ER or urgent care. FUNDING AGENCIES: None

Published
2018
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10. A237 COLONOSCOPY PREPARATION OPTIMIZATION FOR INPATIENTS (COIN STUDY). A RANDOMIZED CONTROLLED TRIAL COMPARING 4L PEGLYTE TO REGULAR DOSE PICO SALAX AND SPLIT DOSE PICO SALAX FOR COLONOSCOPY BOWEL PREPARATION IN HOSPITALIZED PATIENTS

Author

H Fergani, R Spaziani, David Morgan, Subhas C. Ganguli, Keith Tsoi, S. Jalali, Khurram J. Khan, A Merali, and N Forbes

Subjects
medicine.medical_specialty, Ileus, medicine.diagnostic_test, business.industry, medicine.medical_treatment, Pico-Salax, Colonoscopy, Bowel resection, medicine.disease, Paper Sessions, Surgery, law.invention, Randomized controlled trial, law, Split dose, medicine, Bowel preparation, Bisacodyl, business, medicine.drug
Abstract

BACKGROUND: Colonoscopy is routinely performed in hospitalized patients (HP) for investigation and treatment. Being a HP is a risk factor for a poor bowel preparation but there are limited studies examining bowel cleansing in this population. AIMS: Our goal was to determine whether a low volume prep (PicoSalax) taken the day before or as a split prep is superior to a 4L of PegLyte taken the day before colonoscopy. METHODS: This single-centre, endoscopist-blinded, three armed randomized controlled trial compared 4L PEG-Lyte to regular dose Pico Salax and to split dose Pico-Salax for colonoscopy preparation in HP’s. In addition, all patients were given Bisacodyl before starting the preparation. Inclusion criteria: Adult in-patients requiring colonoscopy. Exclusion criteria: renal insufficiency, severe congestive heart failure, recent myocardial infarction, ileus, ascites, severe colitis, megacolon, gastrointestinal obstruction, presence feeding tube, bowel resection, pregnancy, or allergy to study drugs. The primary outcome was overall cleansing efficacy using the Ottawa Bowel Preparation Scale (OBPS) as determined by the endoscopist. Secondary outcomes were components of the OBPS, canceled or repeated procedure due to poor cleansing, and safety and tolerability. The study sample size was calculated to be 126 patients. RESULTS: From October 2012 to November 2016, 44 patients were recruited and randomized. One patient refused to take the preparation. One patient’s procedure was canceled, and one patient was un-blinded due to poor response. The average patient age was 65.7 year’s with 22 females (50%). Indications for colonoscopy include investigation of bleeding (18), anemia (13), change in bowels (6), and abnormal imaging (2). There were 16 patients in the Pico Salax day before group, with mean OBPS of 6.5 (standard deviation (SD) 3.4), 13 patients in the Pico Salax split dose group, with mean OBPS of 4.3 (SD 2.6), and 15 patients in the PEGLyte group, with mean OBPS of 4.9 (SD 2.9) with ANOVA showing no difference between groups (p=0.15). Four patients reported severe adverse effects while taking the prep. Bowel preparation did not result in any cancelation or repeat procedure. The study was terminated early due to poor recruitment. CONCLUSIONS: Preparing hospitalized patients for colonoscopy is a challenging task. The optimal bowel preparation for these patients remains unknown. This study did not show any meaningful difference between groups taking PicoSalax the day before colonoscopy, or Pico Salax as a split preparation, or PEG Lyte the day before colonoscopy but was limited in power because of poor recruitment. Further research is needed in this population. FUNDING AGENCIES: Resident Research Grant, Department of Medicine, McMaster University.

Published
2018
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11. Measurement of dissolved in water at the Sudbury Neutrino Observatory

Author

M. Liu, H.W. Lee, K. McFarlane, I. Blevis, R. L. Hahn, I. Levine, X Zhu, E. Bonvin, S. Majerus, J. Boger, P. Jagam, A. B. Knox, David A. Sinclair, H. Fergani, J. K. Rowley, J. J. Simpson, H. Heron, C. K. Hargrove, A.S Hamer, J.-X Wang, Bhaskar Sur, S Noël, Minfang Yeh, V. M. Novikov, B. T. Cleveland, Darren Grant, N. A. Jelley, J. Farine, A. J. Noble, G. Doucas, A. B. McDonald, F. Dalnoki-Veress, C. Jillings, M. Shatkay, X Dai, and C. Mifflin

Subjects
Heavy water, Physics, Nuclear and High Energy Physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Degasser, Solar neutrino, Analytical chemistry, chemistry.chemical_element, Radon, Lucas cell, 7. Clean energy, 01 natural sciences, 6. Clean water, Nuclear physics, chemistry.chemical_compound, chemistry, 0103 physical sciences, 010306 general physics, Instrumentation, Water vapor, Cold trap
Abstract

The technique used at the Sudbury Neutrino Observatory (SNO) to measure the concentration of 222 Rn 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 222 Rn 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 H2O 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.

Published
2004
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12. Combined analysis of all three phases of solar neutrino data from the Sudbury Neutrino Observatory

Author

M. Kos, Peter Watson, L. L. Kormos, Jocelyn Monroe, B. C. Robertson, G. T. Ewan, K. Boudjemline, M. H. Schwendener, M. Huang, E. Guillian, B. Aharmim, T. Kutter, B. G. Nickel, P. J. Doe, F. Zhang, J. R. Leslie, A. W. P. Poon, M. Bergevin, N. Gagnon, J. Law, G. D. Orebi Gann, P.-L. Drouin, Yuen-Dat Chan, K. Graham, F. A. Duncan, S. M. Oser, Hal Evans, N. McCauley, M. L. Miller, B. Beltran, G. Prior, S. D. Reitzner, S. N. Ahmed, R. D. Martin, H. Deng, Christopher C. M. Kyba, Steven Elliott, R. G. H. Robertson, R. J. Ford, C. Kraus, T. Sonley, R. Van Berg, Kai Zuber, P. Jagam, Rachel Rosten, M. Dunford, J. Wendland, S. J. M. Peeters, Olivier Simard, Keith Rielage, A. L. Hallin, A. Krüger, J. F. Wilkerson, G. Doucas, R. W. Ollerhead, A. Hime, N. West, A. J. Noble, C. B. Krauss, W. J. Heintzelman, F. Fleurot, A. E. Anthony, H. Wan Chan Tseung, M. L. Chen, S. Habib, Bei Cai, H. M. O'Keeffe, K. T. Lesko, D. L. Wark, D. Chauhan, Joseph A. Formaggio, Minfang Yeh, J. M. Wouters, Ryuta Hazama, B. T. Cleveland, S. Majerus, J. C. Loach, N. A. Jelley, H. B. Mak, J. Maneira, M. Jerkins, N. Tolich, J. J. Simpson, G. Tešić, J. Tm. Goon, A. B. McDonald, S. McGee, R. L. Hahn, S. D. Biller, R. A. Ott, P. J. Harvey, C. J. Virtue, E. D. Hallman, N. Barros, B.A. VanDevender, C. Howard, J. Farine, J. R. Wilson, J. Heise, T. Tsui, E. W. Beier, M. DiMarco, B. Jamieson, S. Seibert, R. MacLellan, N. S. Oblath, Mark Guy Boulay, R. L. Helmer, J. R. Klein, P. Skensved, X. Dai, J. A. Detwiler, R. Lange, J. A. Secrest, I. T. Lawson, L. C. Stonehill, G. A. Cox, Benjamin Monreal, E. D. Earle, K. J. Keeter, A. Wright, H. Fergani, and Alain Bellerive

Subjects
Nuclear and High Energy Physics, Particle physics, Solar neutrino, FOS: Physical sciences, Cosmic ray, 7. Clean energy, 01 natural sciences, Particle identification, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Nuclear Experiment (nucl-ex), 010306 general physics, Neutrino oscillation, Nuclear Experiment, Charged current, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Sudbury Neutrino Observatory, Neutral current, 010308 nuclear & particles physics, QC0793, High Energy Physics - Phenomenology, Astrophysics - Solar and Stellar Astrophysics, Neutrino
Abstract

We report results from a combined analysis of solar neutrino data from all phases of the Sudbury Neutrino Observatory. By exploiting particle identification information obtained from the proportional counters installed during the third phase, this analysis improved background rejection in that phase of the experiment. The combined analysis resulted in a total flux of active neutrino flavors from 8B decays in the Sun of (5.25 \pm 0.16(stat.)+0.11-0.13(syst.))\times10^6 cm^{-2}s^{-1}. A two-flavor neutrino oscillation analysis yielded \Deltam^2_{21} = (5.6^{+1.9}_{-1.4})\times10^{-5} eV^2 and tan^2{\theta}_{12}= 0.427^{+0.033}_{-0.029}. A three-flavor neutrino oscillation analysis combining this result with results of all other solar neutrino experiments and the KamLAND experiment yielded \Deltam^2_{21} = (7.41^{+0.21}_{-0.19})\times10^{-5} eV^2, tan^2{\theta}_{12} = 0.446^{+0.030}_{-0.029}, and sin^2{\theta}_{13} = (2.5^{+1.8}_{-1.5})\times10^{-2}. This implied an upper bound of sin^2{\theta}_{13} < 0.053 at the 95% confidence level (C.L.).

Published
2013

13. Measurement of theνeand total8B solar neutrino fluxes with the Sudbury Neutrino Observatory phase-III data set

Author

M. DiMarco, R. J. Ford, R. W. Ollerhead, R. MacLellan, Mark Guy Boulay, P. Jagam, M. H. Schwendener, A. Krüger, B. C. Robertson, J. Tm. Goon, N. Gagnon, G. Doucas, F. Zhang, J. R. Wilson, J. B. Wilhelmy, S. Habib, R. L. Helmer, S. R. Seibert, J. Law, T. Kutter, J. Heise, N. West, P.-L. Drouin, P. Skensved, Hal Evans, F. Fleurot, G. D. Orebi Gann, J. F. Amsbaugh, Ryuta Hazama, H. Wan Chan Tseung, M. L. Miller, A. E. Anthony, J. V. Germani, E. D. Hallman, W. J. Heintzelman, H. Deng, K. M. Heeger, E. Guillian, C. Kraus, S. D. Biller, J. R. Leslie, S. Majerus, Yuen-Dat Chan, K. Boudjemline, K. Graham, M. W.E. Smith, L. L. Kormos, Alain Bellerive, Bernie G. Nickel, J. Wendland, S. M. Oser, S. R. Elliott, G. T. Ewan, Andrew Hime, Joshua R. Klein, A. W. Myers, P. J. Harvey, Juan-Manuel Anaya, J. Banar, K. T. Lesko, Monica Dunford, J. Maneira, M. A. Howe, M. Huang, Reyco Henning, P. M. Thornewell, N. Barros, T. J. Sonley, A. W. P. Poon, S. D. Reitzner, S. N. Ahmed, R. D. Martin, J. J. Simpson, Malcolm M. Fowler, Kai Zuber, T. J. Bowles, C. D. Tunnell, P. J. Doe, G. Tešić, J. A. Formaggio, M. Bergevin, C. A. Duba, N. McCauley, A. Goldschmidt, Bei Cai, Minfang Yeh, E. Rollin, R. G. H. Robertson, R. A. Ott, T.H. Burritt, D. Chauhan, R. Van Berg, H. B. Mak, C. J. Virtue, B. Jamieson, J. F. Wilkerson, T. D. Van Wechel, K. J. Keeter, A. Wright, J. C. Loach, C. Currat, N. A. Jelley, S. J. M. Peeters, T. D. Steiger, M. L. Chen, T. V. Bullard, M. Kos, A. A. Hamian, O. Simard, X. Dai, J. A. Detwiler, R. Lange, G. Prior, C. Howard, E. W. Beier, J. Farine, R. L. Hahn, M. C. Browne, A. J. Noble, L. C. Stonehill, S. McGee, J. M. Wouters, A. B. McDonald, Christopher C. M. Kyba, B. L. Wall, B. T. Cleveland, H. M. O'Keeffe, Keith Rielage, Jocelyn Monroe, B. Aharmim, B. Beltran, A. L. Hallin, C. Mifflin, N. S. Oblath, C. B. Krauss, M. R. Dragowsky, B. A. VanDevender, N. Tolich, Guthrie Miller, B. Morissette, Benjamin Monreal, E. D. Earle, G. C. Harper, F. A. Duncan, J. A. Secrest, I. T. Lawson, D. Waller, G. A. Cox, H. Fergani, and T. Tsui

Subjects
Physics, Nuclear and High Energy Physics, Sudbury Neutrino Observatory, Solar energetic particles, 010308 nuclear & particles physics, Solar neutrino, Cosmic ray, 01 natural sciences, 7. Clean energy, Nuclear physics, 0103 physical sciences, Neutrino, 010306 general physics, Neutrino oscillation, Charged current, Lepton
Abstract

This paper details the solar neutrino analysis of the 385.17-day phase-III data set acquired by the Sudbury Neutrino Observatory (SNO). An array of He-3 proportional counters was installed in the heavy-water target to measure precisely the rate of neutrino-deuteron neutral-current interactions. This technique to determine the total active B-8 solar neutrino flux was largely independent of the methods employed in previous phases. The total flux of active neutrinos was measured to be 5.54(-0.31)(+0.33)(stat.)(-0.34)(+0.36)(syst.) x 10(6) cm(-2) s(-1), consistent with previous measurements and standard solar models. A global analysis of solar and reactor neutrino mixing parameters yielded the best-fit values of Delta m(2) = 7.59(-0.21)(+0.19) x 10(-5) eV(2) and theta = 34.4(-1.2)(+1.3) degrees. DOI: 10.1103/PhysRevC.87.015502

Published
2013
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14. A Search for Astrophysical Burst Signals at the Sudbury Neutrino Observatory

Author

P. Skensved, Monica Dunford, J. Maneira, S. J. M. Peeters, A. W. P. Poon, J. Tm. Goon, Jocelyn Monroe, J. A. Secrest, I. T. Lawson, S. Habib, J. Wendland, C. J. Virtue, G. Prior, N. Barros, D. Waller, Yuen-Dat Chan, K. Graham, David A. Sinclair, T. Tsui, G. A. Cox, Kai Zuber, Joseph A. Formaggio, J. Heise, Christopher C. M. Kyba, A. Wright, X. Dai, Minfang Yeh, E. D. Hallman, K. Boudjemline, M. DiMarco, F. Fleurot, J. A. Detwiler, R. Lange, S. M. Oser, Benjamin Monreal, B. Aharmim, E. D. Earle, J. C. Loach, N. A. Jelley, O. Simard, I. Levine, D. Chauhan, C. Kraus, A. E. Anthony, B. Beltran, M. L. Miller, K. J. Keeter, B. C. Robertson, S. D. Reitzner, S. N. Ahmed, S. Majerus, J. F. Wilkerson, N. West, G. Doucas, M. Bergevin, C. B. Krauss, N. S. Oblath, A. Krueger, W. J. Heintzelman, T. Kutter, J. J. Simpson, R. A. Ott, M. H. Schwendener, N. McCauley, T. J. Sonley, P. J. Doe, H. Fergani, P. Jagam, F. Zhang, A. L. Hallin, R. L. Hahn, Keith Rielage, K. T. Lesko, Peter Watson, Alain Bellerive, R. Van Berg, R. J. Ford, Bei Cai, J. Law, N. Tolich, J. R. Wilson, M. Kos, B. T. Cleveland, P.-L. Drouin, R. MacLellan, S. R. Seibert, E. W. Beier, Mark Guy Boulay, Min Chen, H. Wan Chan Tseung, Steven Elliott, L. C. Stonehill, D. L. Wark, Hal Evans, J. M. Wouters, Joshua R. Klein, J. R. Leslie, E. Guillian, A. B. McDonald, B.A. VanDevender, Andrew Hime, C. Howard, J. Farine, A. J. Noble, M. Jerkins, F. A. Duncan, M. Huang, Miriam Diamond, G. Tešić, R. D. Martin, R. G. H. Robertson, H. B. Mak, L. L. Kormos, S. McGee, G. T. Ewan, B. L. Wall, N. Gagnon, R. Hazama, G. D. Orebi Gann, H. Deng, H. M. O'Keeffe, S. D. Biller, R. L. Helmer, Bernie G. Nickel, P. J. Harvey, R.W. Ollerhead, B. Jamieson, Massachusetts Institute of Technology. Department of Physics, Massachusetts Institute of Technology. Laboratory for Nuclear Science, Formaggio, Joseph A., Miller, Michael L., Monreal, Benjamin, Monroe, Jocelyn, Solomon-Oblath, Noah, Ott, Richard A., and Sonley, Thomas J.

Subjects
Physics, Sudbury Neutrino Observatory, Physics::Instrumentation and Detectors, Solar neutrino, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Phenomenology, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Solar neutrino problem, Neutrino detector, Astrophysics - Solar and Stellar Astrophysics, Measurements of neutrino speed, Astrophysics::Solar and Stellar Astrophysics, High Energy Physics::Experiment, Neutrino astronomy, Neutrino, Nuclear Experiment (nucl-ex), Neutrino oscillation, Nuclear Experiment, QC, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The Sudbury Neutrino Observatory (SNO) has confirmed the standard solar model and neutrino oscillations through the observation of neutrinos from the solar core. In this paper we present a search for neutrinos associated with sources other than the solar core, such as gamma-ray bursts and solar flares. We present a new method for looking for temporal coincidences between neutrino events and astrophysical bursts of widely varying intensity. No correlations were found between neutrinos detected in SNO and such astrophysical sources., United States. Dept. of Energy, National Energy Research Scientific Computing Center (U.S.), Alfred P. Sloan Foundation

Published
2013
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15. LOW-MULTIPLICITY BURST SEARCH AT THE SUDBURY NEUTRINO OBSERVATORY

Author

J. A. Secrest, G. T. Ewan, E. Guillian, B. C. Robertson, G. Doucas, T. Kutter, S. D. Biller, J. J. Simpson, Bernie G. Nickel, F. Fleurot, A. E. Anthony, P. J. Harvey, N. West, C. J. Virtue, T. Tsui, W. J. Heintzelman, R. A. Ott, Benjamin Monreal, E. D. Earle, M. Huang, K. T. Lesko, K. Boudjemline, Monica Dunford, N. Barros, Hal Evans, E. D. Hallman, M. L. Miller, J. Maneira, S. R. Seibert, Christopher C. M. Kyba, B. Beltran, A. W. P. Poon, T. J. Sonley, Keith Rielage, M. Kos, S. D. Reitzner, S. N. Ahmed, Joseph A. Formaggio, R. D. Martin, Minfang Yeh, J. R. Wilson, G. Prior, R. G. H. Robertson, Joshua R. Klein, J. R. Leslie, J. Heise, J. C. Loach, N. A. Jelley, N. Gagnon, G. Tešić, H. M. O'Keeffe, R. J. Ford, H. Fergani, A. Wright, R. Hazama, G. D. Orebi Gann, Bei Cai, E. W. Beier, S. Habib, A. L. Hallin, Steven Elliott, R. MacLellan, R. L. Helmer, H. Deng, Jocelyn Monroe, H. B. Mak, B.A. VanDevender, Mark Guy Boulay, O. Simard, C. Howard, J. Farine, B. Aharmim, M. Jerkins, A. J. Noble, C. B. Krauss, N. S. Oblath, J. F. Wilkerson, David A. Sinclair, S. J. M. Peeters, C. Kraus, Peter Watson, J. T.M. Goon, Yuen-Dat Chan, F. A. Duncan, K. Graham, D. Chauhan, S. M. Oser, N. Tolich, P. Skensved, A. B. McDonald, L. C. Stonehill, and K. Zuber, R. L. Hahn, H. Wan Chan Tseung, B. T. Cleveland, M. Bergevin, Alain Bellerive, X. Dai, J. A. Detwiler, N. McCauley, R. Van Berg, B. Jamieson, M. L. Chen, S. Majerus, Andrew Hime, M. H. Schwendener, F. Zhang, J. Law, and P.-L. Drouin

Subjects
Physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Detector, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Elementary particle, Astrophysics, 01 natural sciences, High Energy Physics - Experiment, Massless particle, High Energy Physics - Experiment (hep-ex), Supernova, Space and Planetary Science, 0103 physical sciences, Neutrino, Multiplicity (chemistry), 010306 general physics
Abstract

Results are reported from a search for low-multiplicity neutrino bursts in the Sudbury Neutrino Observatory (SNO). Such bursts could indicate detection of a nearby core-collapse supernova explosion. The data were taken from Phase I (November 1999 - May 2001), when the detector was filled with heavy water, and Phase II (July 2001 - August 2003), when NaCl was added to the target. The search was a blind analysis in which the potential backgrounds were estimated and analysis cuts were developed to eliminate such backgrounds with 90% confidence before the data were examined. The search maintained a greater than 50% detection probability for standard supernovae occurring at a distance of up to 60 kpc for Phase I and up to 70 kpc for Phase II. No low-multiplicity bursts were observed during the data-taking period., 11 pages, 4 figures, submitted to ApJ

Published
2011

16. Low-energy-threshold analysis of the Phase I and Phase II data sets of the Sudbury Neutrino Observatory

Author

Monica Dunford, J. Maneira, A. W. P. Poon, Christopher C. M. Kyba, J. R. Leslie, J. Tm. Goon, J. F. Wilkerson, Joseph A. Formaggio, M. Kos, Minfang Yeh, C. J. Virtue, C. B. Krauss, N. S. Oblath, M. L. Miller, E. W. Beier, J. C. Loach, B. Beltran, R. A. Ott, R. D. Martin, H. B. Mak, N. A. Jelley, Jocelyn Monroe, N. Gagnon, Andrew Hime, I. Levine, R. G. H. Robertson, E. D. Hallman, M. Huang, G. Tešić, F. A. Duncan, Howe, F. Fleurot, R. Hazama, Yuen-Dat Chan, K. Graham, A. L. Hallin, J. R. Wilson, Kai Zuber, C. D. Tunnell, S. McGee, B. C. Robertson, A. E. Anthony, S. M. Oser, G. D. Orebi Gann, S. D. Biller, N. Barros, Bernie G. Nickel, B. Aharmim, G. Doucas, A. B. McDonald, C. Kraus, S. J. M. Peeters, P. J. Harvey, J.M. Wouters, R. L. Hahn, H. Deng, T. Tsui, S. Habib, N. Tolich, T. Kutter, P. Skensved, M. DiMarco, Steven Elliott, B.A. VanDevender, P. J. Doe, R. J. Ford, M. H. Schwendener, F. Zhang, J. Law, B. L. Wall, Hal Evans, David A. Sinclair, H. M. O'Keeffe, K. Boudjemline, N. West, W. J. Heintzelman, K. T. Lesko, C. Howard, J. Farine, A. J. Noble, B. Morissette, Keith Rielage, K. J. Keeter, T. J. Sonley, Bei Cai, E. Guillian, R. MacLellan, D. Chauhan, Mark Guy Boulay, L. L. Kormos, P.-L. Drouin, B. Jamieson, R. L. Helmer, G. T. Ewan, S. D. Reitzner, S. N. Ahmed, S. R. Seibert, J. Heise, X. Dai, J. A. Detwiler, C. A. Duba, H. Fergani, J. A. Secrest, I. T. Lawson, D. Waller, G. A. Cox, Benjamin Monreal, E. D. Earle, H. Wan Chan Tseung, D. L. Wark, G. Prior, T.H. Burritt, B. T. Cleveland, A. Wright, O. Simard, Alain Bellerive, L. C. Stonehill, M. Bergevin, N. McCauley, R. Van Berg, M. L. Chen, S. Majerus, and Joshua R. Klein

Subjects
Nuclear and High Energy Physics, Particle physics, Solar neutrino, FOS: Physical sciences, 7. Clean energy, 01 natural sciences, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Nuclear Experiment (nucl-ex), 010306 general physics, Neutrino oscillation, Nuclear Experiment, Charged current, Physics, Research Groups and Centres\Physics\Low Temperature Physics, Sudbury Neutrino Observatory, Faculty of Science\Physics, 010308 nuclear & particles physics, Solar neutrino problem, High Energy Physics - Phenomenology, 13. Climate action, Measurements of neutrino speed, High Energy Physics::Experiment, Neutrino, Lepton
Abstract

Results are reported from a joint analysis of Phase I and Phase II data from the Sudbury Neutrino Observatory. The effective electron kinetic energy threshold used is T_eff=3.5 MeV, the lowest analysis threshold yet achieved with water Cherenkov detector data. In units of 10^6 cm^{-2} s^{-1}, the total flux of active-flavor neutrinos from 8B decay in the Sun measured using the neutral current (NC) reaction of neutrinos on deuterons, with no constraint on the 8B neutrino energy spectrum, is found to be Phi_NC = 5.140 ^{+0.160}_{-0.158} (stat) ^{+0.132}_{-0.117} (syst). These uncertainties are more than a factor of two smaller than previously published results. Also presented are the spectra of recoil electrons from the charged current reaction of neutrinos on deuterons and the elastic scattering of electrons. A fit to the SNO data in which the free parameters directly describe the total 8B neutrino flux and the energy-dependent nu_e survival probability provides a measure of the total 8B neutrino flux Phi_8B = 5.046 ^{+0.159}_{-0.152} (stat) ^{+0.107}_{-0.123} (syst). Combining these new results with results of all other solar experiments and the KamLAND reactor experiment yields best-fit values of the mixing parameters of theta_{12}=34.06 ^{+1.16}_{-0.84} degrees and Delta m^2_{21}=7.59 ^{+0.20}_{-0.21} x 10^{-5} eV^2. The global value of Phi_8B is extracted to a precision of ^{+2.38}_{-2.95} %. In a three-flavor analysis the best fit value of sin^2\theta_{13} is 2.00 ^{+2.09}_{-1.63} x 10^{-2}. Interpreting this as a limit implies an upper bound of sin^2\theta_{13} < 0.057 (95% C. L.)., Comment: 53 pages, 40 figures, submitted to Phys. Rev. C

Published
2010
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17. Measurement of the cosmic ray and neutrino-induced muon flux at the Sudbury neutrino observatory

Author

I. Levine, H. M. O'Keeffe, M. L. Miller, R. D. Martin, R. G. H. Robertson, X. Dai, J. A. Detwiler, Keith Rielage, T.H. Burritt, J. R. Leslie, T. J. Sonley, R. Lange, Christopher C. M. Kyba, S. N. Ahmed, Bei Cai, Yuen-Dat Chan, K. Graham, S. M. Oser, Jocelyn Monroe, N. Barros, S. R. Seibert, Reyco Henning, M.G. Boulay, C. A. Currat, N. Gagnon, G. T. Ewan, R. Hazama, M. A. Howe, M. Huang, G. D. Orebi Gann, B. Aharmim, M. W.E. Smith, H. Deng, P. Skensved, C. K. Hargrove, T. Tsui, H. B. Mak, M. Bergevin, H. Wan Chan Tseung, K. Boudjemline, J. R. Wilson, C. E. Okada, J. J. Simpson, Chris Waltham, S. Habib, D. L. Wark, G. Tešić, C. Kraus, A. Wright, David A. Sinclair, O. Simard, J. Wendland, Steven Elliott, A. D. Marino, N. McCauley, S. McGee, G. Prior, S. D. Biller, Y. Opachich, P. J. Harvey, J. M. Wouters, C. B. Krauss, N. S. Oblath, Alain Bellerive, J. F. Wilkerson, S. J. M. Peeters, J. T.M. Goon, Darren Grant, B. Jamieson, Hal Evans, L. C. Stonehill, B. T. Cleveland, R. L. Helmer, A. B. McDonald, E. Guillian, C. J. Virtue, E. D. Hallman, T. C. Andersen, Monica Dunford, J. Maneira, R. L. Hahn, A. W. P. Poon, B. C. Robertson, G. Doucas, P. J. Doe, R. A. Ott, K. M. Heeger, T. D. Steiger, T. Kutter, M. L. Chen, R. J. Ford, B.A. VanDevender, R. MacLellan, Joseph A. Formaggio, C. Howard, J. Farine, Minfang Yeh, A. J. Noble, J. C. Loach, N. A. Jelley, S. Majerus, Joshua R. Klein, R. S. Dosanjh, Andrew Hime, E. Rollin, M. C. Chon, J. A. Secrest, I. T. Lawson, R. J. Hemingway, M. Kos, B. Beltran, E. W. Beier, D. Waller, A. L. Hallin, C. Mifflin, Kai Zuber, N. West, W. J. Heintzelman, H. Fergani, K. T. Lesko, Benjamin Monreal, N. Tagg, M. H. Schwendener, F. A. Duncan, F. Zhang, J. Law, P.-L. Drouin, Peter Watson, N. Tolich, G.A. Cox-Mobrand, F. Dalnoki-Veress, A. Krüger, R. G. Van de Water, J. Heise, F. Fleurot, A. E. Anthony, and S. Luoma

Subjects
Nuclear and High Energy Physics, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Cosmic ray, Astrophysics, 01 natural sciences, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), 0103 physical sciences, Nuclear Experiment (nucl-ex), Nuclear Experiment, 010306 general physics, Neutrino oscillation, Zenith, Physics, Sudbury Neutrino Observatory, Research Groups and Centres\Physics\Low Temperature Physics, Muon, 010308 nuclear & particles physics, Faculty of Science\Physics, High Energy Physics::Phenomenology, Astrophysics::Instrumentation and Methods for Astrophysics, High Energy Physics::Experiment, Neutrino, Lepton
Abstract

Results are reported on the measurement of the atmospheric neutrino-induced muon flux at a depth of 2 kilometers below the Earth's surface from 1229 days of operation of the Sudbury Neutrino Observatory (SNO). By measuring the flux of through-going muons as a function of zenith angle, the SNO experiment can distinguish between the oscillated and un-oscillated portion of the neutrino flux. A total of 514 muon-like events are measured between $-1 \le \cos{\theta}_{\rm zenith} \le 0.4$ in a total exposure of 2.30\times 10^{14}$ cm$^{2}$ s. The measured flux normalization is $1.22 \pm 0.09$ times the Bartol three-dimensional flux prediction. This is the first measurement of the neutrino-induced flux where neutrino oscillations are minimized. The zenith distribution is consistent with previously measured atmospheric neutrino oscillation parameters. The cosmic ray muon flux at SNO with zenith angle $\cos{\theta}_{\rm zenith} > 0.4$ is measured to be $(3.31 \pm 0.01 {\rm (stat.)} \pm 0.09 {\rm (sys.)}) \times 10^{-10}~\mu$/s/cm$^{2}$., Comment: 17 pages, 11 figures

Published
2009

18. High sensitivity measurement of 224Ra and 226Ra in water with an improved hydrous titanium oxide technique at the Sudbury Neutrino Observatory

Author

H. Fergani, X. Dai, R. J. Ford, R. Lange, J. Farine, A. J. Noble, G. Doucas, S. Majerus, E. D. Hallman, C. Mifflin, David A. Sinclair, H. M. O'Keeffe, Minfang Yeh, N. A. Jelley, B. Aharmim, R. L. Hahn, R. Rodriguez-jimenez, and B. T. Cleveland

Subjects
Heavy water, Physics, Nuclear and High Energy Physics, Sudbury Neutrino Observatory, Alkaline earth metal, 010308 nuclear & particles physics, Liquid scintillation counting, Analytical chemistry, FOS: Physical sciences, Thorium, chemistry.chemical_element, Uranium, 01 natural sciences, 7. Clean energy, Titanium oxide, Nuclear physics, chemistry.chemical_compound, chemistry, 13. Climate action, 0103 physical sciences, Nuclear Experiment (nucl-ex), 010306 general physics, Instrumentation, Nuclear Experiment, Isotopes of thorium
Abstract

The existing hydrous titanium oxide (HTiO) technique for the measurement of 224Ra and 226Ra in the water at the Sudbury Neutrino Observatory (SNO) has been changed to make it faster and less sensitive to trace impurities in the HTiO eluate. Using HTiO-loaded filters followed by cation exchange adsorption and HTiO co-precipitation, Ra isotopes from 200-450 tonnes of heavy water can be extracted and concentrated into a single sample of a few millilitres with a total chemical efficiency of 50%. Combined with beta-alpha coincidence counting, this method is capable of measuring 2.0x10^3 uBq/kg of 224Ra and 3.7x10^3 uBq/kg of 226Ra from the 232Th and 238U decay chains, respectively, for a 275 tonne D2O assay, which are equivalent to 5x10^16 g Th/g and 3x10^16 g U/g in heavy water., 8 Pages, 2 figures and 2 tables

Published
2008

19. Independent measurement of the total active 8B solar neutrino flux using an array of 3He proportional counters at the sudbury neutrino observatory

Author

B, Aharmim, S N, Ahmed, J F, Amsbaugh, A E, Anthony, J, Banar, N, Barros, E W, Beier, A, Bellerive, B, Beltran, M, Bergevin, S D, Biller, K, Boudjemline, M G, Boulay, T J, Bowles, M C, Browne, T V, Bullard, T H, Burritt, B, Cai, Y D, Chan, D, Chauhan, M, Chen, B T, Cleveland, G A, Cox-Mobrand, C A, Currat, X, Dai, H, Deng, J, Detwiler, M, DiMarco, P J, Doe, G, Doucas, P-L, Drouin, C A, Duba, F A, Duncan, M, Dunford, E D, Earle, S R, Elliott, H C, Evans, G T, Ewan, J, Farine, H, Fergani, F, Fleurot, R J, Ford, J A, Formaggio, M M, Fowler, N, Gagnon, J V, Germani, A, Goldschmidt, J T M, Goon, K, Graham, E, Guillian, S, Habib, R L, Hahn, A L, Hallin, E D, Hallman, A A, Hamian, G C, Harper, P J, Harvey, R, Hazama, K M, Heeger, W J, Heintzelman, J, Heise, R L, Helmer, R, Henning, A, Hime, C, Howard, M A, Howe, M, Huang, P, Jagam, B, Jamieson, N A, Jelley, K J, Keeter, J R, Klein, L L, Kormos, M, Kos, A, Krüger, C, Kraus, C B, Krauss, T, Kutter, C C M, Kyba, R, Lange, J, Law, I T, Lawson, K T, Lesko, J R, Leslie, J C, Loach, R, MacLellan, S, Majerus, H B, Mak, J, Maneira, R, Martin, K, McBryde, N, McCauley, A B, McDonald, S, McGee, C, Mifflin, G G, Miller, M L, Miller, B, Monreal, J, Monroe, B, Morissette, A, Myers, B G, Nickel, A J, Noble, N S, Oblath, H M, O'Keeffe, R W, Ollerhead, G D Orebi, Gann, S M, Oser, R A, Ott, S J M, Peeters, A W P, Poon, G, Prior, S D, Reitzner, K, Rielage, B C, Robertson, R G H, Robertson, E, Rollin, M H, Schwendener, J A, Secrest, S R, Seibert, O, Simard, J J, Simpson, L, Sinclair, P, Skensved, M W E, Smith, T D, Steiger, L C, Stonehill, G, Tesić, P M, Thornewell, N, Tolich, T, Tsui, C D, Tunnell, T, Van Wechel, R, Van Berg, B A, VanDevender, C J, Virtue, T J, Walker, B L, Wall, D, Waller, H Wan Chan, Tseung, J, Wendland, N, West, J B, Wilhelmy, J F, Wilkerson, J R, Wilson, J M, Wouters, A, Wright, M, Yeh, F, Zhang, and K, Zuber

Subjects
High Energy Physics::Experiment, Nuclear Experiment, Astrophysics::Galaxy Astrophysics
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_x) 8B solar neutrino flux. This technique is independent of previous methods employed by SNO. The total flux is found to be 5.54_-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_-0.21;+0.19x10(-5) eV2 and theta=34.4_-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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20. An array of low-background $^3$He proportional counters for the Sudbury Neutrino Observatory

Author

C. B. Krauss, N. S. Oblath, S. J. M. Peeters, M. R. Dragowsky, T. V. Bullard, J. Law, J. V. Germani, X. Dai, H. Fergani, A. W. P. Poon, B. Morissette, G. Prior, P. Skensved, J. F. Wilkerson, N. West, J.F. Amsbaugh, R.W. Ollerhead, T. D. Steiger, J. Wendland, Juan-Manuel Anaya, K. T. Lesko, B.A. VanDevender, C. A. Duba, E. Guillian, S. McGee, M. A. Howe, M. Huang, B. L. Wall, I. T. Lawson, J. Manor, S. Majerus, P. J. Doe, M. C. Browne, T. D. Van Wechel, Malcolm M. Fowler, J. M. Wouters, A. Goldschmidt, F. A. Duncan, J. Banar, R. G. H. Robertson, J. B. Wilhelmy, Andrew Hime, Guthrie Miller, G.A. Cox-Mobrand, H. M. O'Keeffe, L. C. Stonehill, Steven Elliott, P. Geissbühler, H. Wan Chan Tseung, M. Di Marco, K.K.S. Miknaitis, Joseph A. Formaggio, Ernst I. Esch, S. D. Reitzner, T. J. Bowles, R. Hazama, E. D. Earle, P. J. Harvey, N. Tolich, P. M. Thornewell, A. L. Hallin, H. Deng, C. Kraus, G. C. Harper, J. C. Loach, L. L. Kormos, Alan R. Smith, T.H. Burritt, J.E. Franklin, K. M. Heeger, J. Heise, A. W. Myers, Keith Rielage, and M. W.E. Smith

Subjects
Physics, Nuclear and High Energy Physics, Sudbury Neutrino Observatory, Physics::Instrumentation and Detectors, 010308 nuclear & particles physics, business.industry, Solar neutrino, Detector, FOS: Physical sciences, Proportional counter, 01 natural sciences, Particle detector, Nuclear physics, Surface coating, Optics, 0103 physical sciences, Neutron detection, High Energy Physics::Experiment, Nuclear Experiment (nucl-ex), Neutrino, Nuclear Experiment, 010306 general physics, business, Instrumentation
Abstract

An array of Neutral-Current Detectors (NCDs) has been built in order to make a unique measurement of the total active flux of solar neutrinos in the Sudbury Neutrino Observatory (SNO). Data in the third phase of the SNO experiment were collected between November 2004 and November 2006, after the NCD array was added to improve the neutral-current sensitivity of the SNO detector. This array consisted of 36 strings of proportional counters filled with a mixture of $^3$He and CF$_4$ gas capable of detecting the neutrons liberated by the neutrino-deuteron neutral current reaction in the D$_2$O, and four strings filled with a mixture of $^4$He and CF$_4$ gas for background measurements. The proportional counter diameter is 5 cm. The total deployed array length was 398 m. The SNO NCD array is the lowest-radioactivity large array of proportional counters ever produced. This article describes the design, construction, deployment, and characterization of the NCD array, discusses the electronics and data acquisition system, and considers event signatures and backgrounds., 32 pages, 18 figures, 6 tables

Published
2007

21. Determination of theνeand totalB8solar neutrino fluxes using the Sudbury Neutrino Observatory Phase I data set

Author

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

Subjects
Physics, Elastic scattering, Nuclear and High Energy Physics, Sudbury Neutrino Observatory, Particle physics, Neutral current, 010308 nuclear & particles physics, Solar neutrino, media_common.quotation_subject, Cosmic ray, 01 natural sciences, 7. Clean energy, Asymmetry, Nuclear physics, 13. Climate action, 0103 physical sciences, Neutrino, 010306 general physics, Charged current, media_common
Abstract

This article provides the complete description of resultsfrom the Phase I data set of the Sudbury Neutrino Observatory (SNO). ThePhase I data set is based on a 0.65 kt-year exposure of heavy water tothe solar 8B neutrino flux. Included here are details of the SNO physicsand detector model, evaluations of systematic uncertainties, andestimates 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 theresults of a search for a day-night asymmetry in the ?e flux. Under theassumption that the 8B spectrum is undistorted, the measurements fromthis phase yield a solar ?e flux of ?(?e) =1.76+0.05?0.05(stat.)+0.09?0.09 (syst.) x 106 cm?2 s?1, and a non-?ecomponent ?(? mu) = 3.41+0.45?0.45(stat.)+0.48?0.45 (syst.) x 106 cm?2s?1. The sum of these components provides a total flux in excellentagreement with the predictions of Standard Solar Models. The day-nightasymmetry in the ?e flux is found to be Ae = 7.0 +- 4.9 (stat.)+1.3?1.2percent (sys.), when the asymmetry in the total flux is constrained to bezero.

Published
2007
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22. A search for neutrinos from the solar hep reaction and the diffuse supernova neutrino background with the Sudbury Neutrino Observatory

Author

S. N. Ahmed, Hal Evans, J. Wendland, A. L. Hallin, C. Mifflin, J. M. Wouters, F. Fleurot, L. L. Kormos, H. Wan Chan Tseung, A. E. Anthony, S. Luoma, H. Labranche, D. L. Wark, G. T. Ewan, R. G. Stokstad, Benjamin Monreal, E. D. Earle, Alain Bellerive, T. Tsui, A. D. Marino, Keith Rielage, F. Dalnoki-Veress, M. DiMarco, P. Jagam, B. C. Robertson, A. Krüger, R. G. Van de Water, G. Doucas, Yuen-Dat Chan, K. Graham, N. Gagnon, J. A. Secrest, I. T. Lawson, S. M. Oser, Joseph A. Formaggio, X. Chen, D. Waller, G. A. Cox, B. L. Wall, R. Hazama, A. Wright, Minfang Yeh, T. Kutter, R. A. Ott, R. J. Ford, P. Skensved, O. Simard, G. D. Orebi Gann, J. C. Loach, N. A. Jelley, B. Aharmim, H. Fergani, R. MacLellan, G. Prior, L. C. Stonehill, H. M. O'Keeffe, H. Deng, C. B. Krauss, N. S. Oblath, S. D. Biller, Bernie G. Nickel, J. R. Wilson, Reyco Henning, R. D. Martin, E. B. Norman, X. Dai, T. J. Walker, M.G. Boulay, R. G. H. Robertson, C. J. Virtue, J. A. Detwiler, M. A. Howe, P. J. Harvey, R. Lange, M. Huang, K. M. Heeger, J. Tm. Goon, N. Tolich, F. A. Duncan, G. Tešić, C. Kraus, J. R. Leslie, B. T. Cleveland, B.A. VanDevender, E. D. Hallman, J. F. Wilkerson, C. Howard, J. Farine, P. J. Doe, A. J. Noble, Joshua R. Klein, J. Heise, J. A. Dunmore, K.K.S. Miknaitis, S. McGee, H. B. Mak, M. Bergevin, N. McCauley, C. A. Currat, R. Van Berg, C. E. Okada, David A. Sinclair, M. L. Chen, S. R. Seibert, S. Majerus, R. L. Helmer, Monica Dunford, J. Maneira, A. W. P. Poon, S. J. M. Peeters, Andrew Hime, M. L. Miller, M. H. Schwendener, F. Zhang, J. Law, P.-L. Drouin, C. J. Sims, Kai Zuber, R. L. Hahn, Christopher C. M. Kyba, E. Rollin, R. J. Hemingway, M. Kos, A. B. McDonald, E. W. Beier, N. West, W. J. Heintzelman, K. T. Lesko, and E. Guillian

Subjects
Physics::Instrumentation and Detectors, Solar neutrino, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 7. Clean energy, 01 natural sciences, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), 0103 physical sciences, Nuclear Experiment (nucl-ex), 010306 general physics, Neutrino oscillation, Nuclear Experiment, Physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Astrophysics (astro-ph), Astronomy and Astrophysics, Solar neutrino problem, Neutrino detector, 13. Climate action, Space and Planetary Science, Measurements of neutrino speed, High Energy Physics::Experiment, Neutrino, Lepton
Abstract

A search has been made for neutrinos from the hep reaction in the Sun and from the diffuse supernova neutrino background (DSNB) using data collected during the first operational phase of the Sudbury Neutrino Observatory, with an exposure of 0.65 kilotonne-years. For the hep neutrino search, two events are observed in the effective electron energy range of 14.3 MeV, Comment: 12 pages, 5 figures, accepted for publication by ApJ. Minor updates to address referees comments

Published
2006
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23. Electron energy spectra, fluxes, and day-night asymmetries of8B solar neutrinos from measurements with NaCl dissolved in the heavy-water detector at the Sudbury Neutrino Observatory

Author

B. Aharmim, S. N. Ahmed, A. E. Anthony, E. W. Beier, A. Bellerive, M. Bergevin, S. D. Biller, J. Boger, M. G. Boulay, M. G. Bowler, T. V. Bullard, Y. D. Chan, M. Chen, X. Chen, B. T. Cleveland, G. A. Cox, C. A. Currat, X. Dai, F. Dalnoki-Veress, H. Deng, P. J. Doe, R. S. Dosanjh, G. Doucas, 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, K. Frame, W. Frati, B. G. Fulsom, N. Gagnon, K. Graham, D. R. Grant, R. L. Hahn, J. C. Hall, A. L. Hallin, E. D. Hallman, W. B. Handler, C. K. Hargrove, P. J. Harvey, R. Hazama, K. M. Heeger, L. Heelan, W. J. Heintzelman, J. Heise, R. L. Helmer, R. J. Hemingway, A. Hime, C. Howard, M. A. Howe, M. Huang, P. Jagam, N. A. Jelley, J. R. Klein, L. L. Kormos, M. S. Kos, A. Krüger, C. Kraus, 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, J. C. Loach, 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, 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, S. J. M. 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, S. R. Seibert, O. Simard, J. J. Simpson, C. J. Sims, D. Sinclair, P. Skensved, M. W. E. Smith, N. Starinsky, R. G. Stokstad, L. C. Stonehill, R. Tafirout, Y. Takeuchi, G. Tešić, M. Thomson, M. Thorman, T. Tsui, R. Van Berg, R. G. Van de Water, C. J. Virtue, B. L. Wall, D. Waller, C. E. Waltham, H. Wan Chan Tseung, D. L. Wark, J. Wendland, N. West, J. F. Wilkerson, J. R. Wilson, P. Wittich, J. M. Wouters, A. Wright, M. Yeh, and K. Zuber

Subjects
Physics, Nuclear reaction, Nuclear and High Energy Physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Solar neutrino, Isotopes of boron, 01 natural sciences, 7. Clean energy, Spectral line, Nuclear physics, 13. Climate action, 0103 physical sciences, High Energy Physics::Experiment, Atomic physics, Neutrino, 010306 general physics, Neutrino oscillation, Lepton
Abstract

Results are reported from the complete salt phase of the Sudbury Neutrino Observatory experiment in which NaCl was dissolved in the {sup 2}H{sub 2}O (''D{sub 2}O'') target. The addition of salt enhanced the signal from neutron capture as compared to the pure D{sub 2}O 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 10{sup 6}cm{sup -2}s{sup -1}, the total flux of active-flavor neutrinos from {sup 8}B decay in the Sun is found to be 4.94{sub -0.21}{sup +0.21}(stat){sub -0.34}{sup +0.38}(syst) and the integral flux of electron neutrinos for an undistorted {sup 8}B spectrum is 1.68{sub -0.06}{sup +0.06}(stat){sub -0.09}{sup +0.08}(syst); the signal from ({nu}{sub x},e) elastic scattering is equivalent to an electron-neutrino flux of 2.35{sub -0.22}{sup +0.22}(stat){sub -0.15}{sup +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 {delta}m{sup 2}=(8.0{sub -0.4}{sup +0.6})x10{sup -5}more » eV{sup 2} and {theta}=33.9{sub -2.2}{sup +2.4} degrees.« less

Published
2005
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24. Search for periodicities in theB8solar neutrino flux measured by the Sudbury Neutrino Observatory

Author

B. Aharmim, S. N. Ahmed, A. E. Anthony, E. W. Beier, A. Bellerive, M. Bergevin, S. D. Biller, M. G. Boulay, M. G. Bowler, Y. D. Chan, M. Chen, X. Chen, B. T. Cleveland, T. Costin, G. A. Cox, C. A. Currat, X. Dai, H. Deng, J. Detwiler, P. J. Doe, R. S. Dosanjh, G. Doucas, 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, W. Frati, B. G. Fulsom, N. Gagnon, J. TM. Goon, K. Graham, R. L. Hahn, A. L. Hallin, E. D. Hallman, W. B. Handler, C. K. Hargrove, P. J. Harvey, R. Hazama, K. M. Heeger, L. Heelan, W. J. Heintzelman, J. Heise, R. L. Helmer, R. J. Hemingway, A. Hime, M. A. Howe, M. Huang, E. Inrig, P. Jagam, N. A. Jelley, J. R. Klein, L. L. Kormos, M. S. Kos, A. Krüger, C. Kraus, 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, J. C. Loach, S. Luoma, R. MacLellan, S. Majerus, J. Maneira, A. D. Marino, N. McCauley, A. B. McDonald, S. McGee, C. Mifflin, K. K. S. Miknaitis, B. G. Nickel, A. J. Noble, E. B. Norman, N. S. Oblath, C. E. Okada, H. M. O’Keeffe, R. W. Ollerhead, G. D. Orebi Gann, J. L. Orrell, S. M. Oser, T. Ouvarova, S. J. M. Peeters, A. W. P. Poon, C. S. J. Pun, K. Rielage, B. C. Robertson, R. G. H. Robertson, E. Rollin, S. S. E. Rosendahl, M. H. Schwendener, S. R. Seibert, O. Simard, J. J. Simpson, C. J. Sims, D. Sinclair, L. Sinclair, P. Skensved, M. W. E. Smith, R. G. Stokstad, L. C. Stonehill, R. Tafirout, Y. Takeuchi, G. Tešić, M. Thomson, K. V. Tsang, T. Tsui, R. Van Berg, C. J. Virtue, B. L. Wall, D. Waller, C. E. Waltham, H. Wan Chan Tseung, D. L. Wark, J. Wendland, N. West, J. F. Wilkerson, J. R. Wilson, J. M. Wouters, M. Yeh, and K. Zuber

Subjects
Physics, Nuclear and High Energy Physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Solar neutrino, Flux, Astrophysics, Solar neutrino problem, 01 natural sciences, Radiation flux, Neutrino detector, 0103 physical sciences, High Energy Physics::Experiment, Neutrino, 010306 general physics, Lepton
Abstract

A search has been made for sinusoidal periodic variations in the 8B 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 8B 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 8B neutrino flux.

Published
2005
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25. Electron antineutrino search at the Sudbury Neutrino Observatory

Author

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

Subjects
Physics, Nuclear reaction, Nuclear and High Energy Physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Flux, FOS: Physical sciences, 7. Clean energy, 01 natural sciences, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), 0103 physical sciences, Neutron, High Energy Physics::Experiment, Neutrino, 010306 general physics, Neutrino oscillation, Nuclear Experiment, Lepton, Bar (unit)
Abstract

Upper limits on the \nuebar flux at the Sudbury Neutrino Observatory have been set based on the \nuebar 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 \nuebar's from the Sun and other potential sources. Both differential and integral limits on the \nuebar flux have been placed in the energy range from 4 -- 14.8 MeV. For an energy-independent ��_e --> \nuebar conversion mechanism, the integral limit on the flux of solar \nuebar's in the energy range from 4 -- 14.8 MeV is found to be ��_\nuebar, submitted to Phys. Rev. D

Published
2004

26. Measurement of the Total ActiveB8Solar Neutrino Flux at the Sudbury Neutrino Observatory with Enhanced Neutral Current Sensitivity

Author

R. L. Helmer, P. J. Doe, R. L. Hahn, Monica Dunford, A. W. P. Poon, R. MacLellan, S. R. Elliott, R. W. Ollerhead, E. D. Hallman, G. T. Ewan, J. Maneira, I. T. Lawson, W. B. Handler, Y. Takeuchi, J. F. Wilkerson, J. Boger, J. J. Simpson, D. Waller, Reda Tafirout, Darren Grant, Christopher C. M. Kyba, Yuen-Dat Chan, B. L. Wall, C. K. Hargrove, P. Skensved, C. E. Okada, David A. Sinclair, G. A. Cox, Eric B. Norman, F. A. Duncan, R. S. Dosanjh, B. A. Moffat, K. Graham, E. Rollin, J. R. Leslie, M. W.E. Smith, B. T. Cleveland, J. M. Wouters, R. G. Stokstad, Chris Waltham, M. A. Howe, Malcolm M. Fowler, C. Ouellet, S. M. Oser, H. Fergani, Guthrie Miller, J. A. Dunmore, J. Farine, A. J. Noble, X. Chen, X. Dai, G. Tešić, N. West, A. V. Krumins, R. Lange, S. J. M. Peeters, V. L. Rusu, K.K.S. Miknaitis, W. J. Heintzelman, M.G. Boulay, S. J. Brice, A. S. Hamer, K. T. Lesko, G. McGregor, A. L. Hallin, J. R. Wilson, C. Mifflin, T. V. Bullard, R. J. Hemingway, S. McGee, M. Kos, E. D. Earle, S. D. Biller, Bernie G. Nickel, H. Wan Chan Tseung, I. Levine, N. S. Oblath, E. W. Beier, C. A. Duba, H. Labranche, A. B. McDonald, D. L. Wark, M. R. Dragowsky, F. Dalnoki-Veress, M. H. Schwendener, M. G. Bowler, A. D. Marino, B. G. Fulsom, J. C. Hall, J. Law, R. G. H. Robertson, C. J. Sims, Kai Zuber, C. W. Nally, Andrew Hime, B. C. Robertson, G. Doucas, J. B. Wilhelmy, T. Kutter, C. J. Virtue, N. Gagnon, John L. Orrell, L. C. Stonehill, S. N. Ahmed, R. Hazama, T. J. Bowles, Joseph A. Formaggio, N. McCauley, Minfang Yeh, N. A. Jelley, M. Thorman, R. Van Berg, O. Simard, Hal Evans, K. Frame, Alain Bellerive, K. M. Heeger, M. L. Chen, M. A. Thomson, J. Heise, F. Fleurot, A. E. Anthony, S. Luoma, P. Jagam, Joshua R. Klein, R. G. Van de Water, N. Starinsky, H. B. Mak, S. S.E. Rosendahl, P. J. Harvey, and S. Majerus

Subjects
Physics, Particle physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Solar neutrino, General Physics and Astronomy, Flux, Cosmic ray, 7. Clean energy, 01 natural sciences, Nuclear physics, Neutrino detector, 13. Climate action, 0103 physical sciences, High Energy Physics::Experiment, Neutrino, 010306 general physics, Neutrino oscillation, Astrophysics::Galaxy Astrophysics, Lepton
Abstract

The Sudbury Neutrino Observatory has precisely determined the total active (nu(x)) B-8 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)x10(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(-0.6)(+1.2)x10(-5) eV(2) and theta= 32.5(-2.3)(+2.4) degrees. Maximal mixing is rejected at the equivalent of 5.4 standard deviations.

Published
2004
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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

S N, Ahmed, A E, Anthony, E W, Beier, A, Bellerive, S D, Biller, J, Boger, M G, Boulay, M G, Bowler, 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, B G, Fulsom, N, Gagnon, K, Graham, D R, Grant, R L, Hahn, J C, Hall, A L, 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, M S, Kos, 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, 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, S J M, Peeters, A W P, Poon, 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, R G, Stokstad, L C, Stonehill, R, Tafirout, Y, Takeuchi, G, Tesić, M, Thomson, M, Thorman, R, Van Berg, R G, Van de Water, C J, Virtue, B L, Wall, D, Waller, C E, Waltham, H Wan Chan, Tseung, D L, Wark, N, West, J B, Wilhelmy, J F, Wilkerson, J R, Wilson, J M, Wouters, M, Yeh, and K, Zuber

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

28. Measurement of day and night neutrino energy spectra at SNO and constraints on neutrino mixing parameters

Author

J. C. Barton, R. L. Helmer, Monica Dunford, A. W. P. Poon, M. Bercovitch, M. Lay, H. Fergani, J. J. Simpson, P. J. Doe, C. J. Virtue, J. A. Dunmore, R. W. Ollerhead, H. Heron, R. U. Haq, J. Lyon, E. D. Earle, B. A. Moffat, I. Levine, T. J. Radcliffe, G. T. Ewan, W. Locke, J. R. Leslie, B. C. Robertson, A. P. Ferraris, J. X. Wang, V. L. Rusu, K. K. Schaffer, S. D. Biller, A. S. Hamer, B. T. Cleveland, T. Kutter, R. Meijer Drees, N. Tagg, F. A. Duncan, R. J. Ford, P. J. Harvey, N. McCauley, M. C.P. Isaac, M. H. Schwendener, N. Gagnon, Xin Chen, E. Bonvin, R. Hazama, E. D. Hallman, A. J. Noble, R. Van Berg, H. S. Ng, P. M. Thornewell, T. D. Steiger, W. J. Heintzelman, M. L. Chen, A. Roberge, K. McFarlane, P. T. Trent, A. A. Hamian, D. F. Cowen, J. Law, C. J. Sims, Joshua R. Klein, J. V. Germani, D. L. Wark, R. G. Van de Water, N. Starinsky, K. T. Lesko, W. Frati, Q. R. Ahmad, Bhaskar Sur, F. Dalnoki-Veress, T. V. Bullard, P. T. Keener, H. B. Mak, A. D. Marino, I. T. Lawson, Richard T. Kouzes, Anett Schulke, J. Bigu, R. J. Boardman, G. A. Cox, E. W. Beier, M. G. Bowler, J. Heise, C. K. Hargrove, G. McGregor, S. Luoma, J. Boger, Y. I. Tserkovnyak, R. G. Stokstad, N.W. Tanner, D. S. McDonald, A. B. McDonald, M. Shatkay, L. C. Stonehill, J. K. Rowley, M. O'Neill, S. S.E. Rosendahl, G. G. Miller, H. W. Lee, V. M. Novikov, C. W. Nally, Christopher C. M. Kyba, Alan R. Smith, M. Moorhead, G. Jonkmans, E. Saettler, S. Majerus, J. Cameron, H. Seifert, Herbert H. Chen, G. Bühler, J. M. Wouters, E. T.H. Clifford, P. Jagam, C. E. Okada, J. D. Hepburn, M. A. Howe, David A. Sinclair, Yuen-Dat Chan, K. Graham, J. Hewett, S. M. Oser, A. L. Hallin, Andrew Hime, J. Manor, C. Mifflin, J. H.M. Cowan, J. Maneira, I. Blevis, R. L. Hahn, Salvador Gil, G. Doucas, M. Omori, M.G. Boulay, C. Jillings, J. F. Wilkerson, Eric B. Norman, J. R. Wilson, K. Frame, Reda Tafirout, Darren Grant, A. B. Knox, C. A. Duba, K. M. Heeger, Hal Evans, John L. Orrell, W. F. Davidson, J. Farine, R. A. Black, W. B. Handler, Joseph A. Formaggio, Minfang Yeh, N. A. Jelley, N. West, M. Thorman, M. W.E. Smith, M. M. Fowler, M. C. Browne, Steven Elliott, T. C. Andersen, E.D. Frank, R. S. Storey, J. G. Hykawy, R. J. Komar, R. C. Allen, P. Skensved, R. K. Taplin, T. J. Bowles, X. Dai, Mark Neubauer, Chris Waltham, G. Milton, R. G. H. Robertson, T. Spreitzer, F.M. Newcomer, J. D. Anglin, S. J. Brice, Peter Wittich, J. B. Wilhelmy, M. R. Dragowsky, K. Kazkaz, Delon, Viviane, Développement et Communication Chimique chez les Insectes ( DCCI ), and Centre National de la Recherche Scientifique ( CNRS ) -Université de Bourgogne ( UB ) -AgroSup Dijon - Institut National Supérieur des Sciences Agronomiques, de l'Alimentation et de l'Environnement

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Solar neutrino, FOS: Physical sciences, General Physics and Astronomy, Flux, Cosmic ray, Astrophysics, 7. Clean energy, 01 natural sciences, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), 0103 physical sciences, Nuclear astrophysics, Nuclear Experiment (nucl-ex), 010306 general physics, Neutrino oscillation, Nuclear Experiment, Astrophysics::Galaxy Astrophysics, Charged current, Physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Astrophysics (astro-ph), High Energy Physics::Phenomenology, 13. Climate action, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Neutrino
Abstract

The Sudbury Neutrino Observatory (SNO) has measured day and night solar neutrino energy spectra and rates. For charged current events, assuming an undistorted $^8$B spectrum, the night minus day rate is $14.0% \pm 6.3% ^{+1.5}_{-1.4}%$ 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 $7.0% \pm 4.9% ^{+1.3}_{-1.2}%$. A global solar neutrino analysis in terms of matter-enhanced oscillations of two active flavors strongly favors the Large Mixing Angle (LMA) solution., Comment: 5 pages, 4 figures; very minor revisions, accepted by Physical Review Letters

Published
2002

29. A radium assay technique using hydrous titanium oxide adsorbent for the Sudbury Neutrino Observatory

Author

T.C Andersen, R.A Black, I Blevis, J Boger, E Bonvin, M Chen, B.T Cleveland, X Dai, F Dalnoki-Veress, G Doucas, J Farine, H Fergani, M.M Fowler, R.L Hahn, E.D Hallman, C.K Hargrove, H Heron, E Hooper, K.H Howard, P Jagam, N.A Jelley, A.B Knox, H.W Lee, I Levine, W Locke, S Majerus, K McFarlane, G McGregor, G.G Miller, M Moorhead, A.J Noble, M Omori, J.K Rowley, M Shatkay, C Shewchuk, J.J Simpson, D Sinclair, N.W Tanner, R.K Taplin, P.T Trent, J.-X Wang, J.B Wilhelmy, and M Yeh

Subjects
Heavy water, Physics, Nuclear and High Energy Physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Solar neutrino, Radiochemistry, Thorium, chemistry.chemical_element, FOS: Physical sciences, Uranium, 7. Clean energy, 01 natural sciences, Radium, chemistry.chemical_compound, chemistry, 0103 physical sciences, Decay chain, Neutrino, Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Experiment, Instrumentation
Abstract

As photodisintegration of deuterons mimics the disintegration of deuterons by neutrinos, the accurate measurement of the radioactivity from thorium and uranium decay chains in the heavy water in the Sudbury Neutrino Observatory (SNO) is essential for the determination of the total solar neutrino flux. A radium assay technique of the required sensitivity is described that uses hydrous titanium oxide adsorbent on a filtration membrane together with a beta-alpha delayed coincidence counting system. For a 200 tonne assay the detection limit for 232Th is a concentration of 3 x 10^(-16) g Th/g water and for 238U of 3 x 10^(-16) g U/g water. Results of assays of both the heavy and light water carried out during the first two years of data collection of SNO are presented., Comment: 12 pages, 4 figures

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

Author

D. S. McDonald, E. D. Earle, J. A. Dunmore, R. U. Haq, Christopher C. M. Kyba, M. C.P. Isaac, V. M. Novikov, T. J. Bowles, G. Jonkmans, E. Saettler, H. Fergani, J. R. Wilson, G. Doucas, E. D. Hallman, M. H. Schwendener, E. Bonvin, R. Hazama, Herbert H. Chen, A. B. Knox, N. McCauley, P. J. Doe, J. Law, P. Jagam, N. W. Tanner, C. J. Sims, J. V. Germani, A. Roberge, H. Heron, A. L. Hallin, R. Van Berg, C. Mifflin, J. B. Wilhelmy, P. T. Trent, H. W. Lee, Joseph A. Formaggio, M. R. Dragowsky, M. M. Fowler, S. D. Biller, J. Hewett, T. V. Bullard, Andrew Hime, T. D. Steiger, R. K. Taplin, M. C. Browne, Minfang Yeh, M. L. Chen, R. L. Hahn, Salvador Gil, K. Kazkaz, A. A. Hamian, J. Farine, G. T. Ewan, K. K. Schaffer, N. A. Jelley, N. West, E. W. Beier, Hal Evans, S. S.E. Rosendahl, E. T.H. Clifford, F.M. Newcomer, M. Lay, R. A. Black, F. A. Duncan, J. D. Anglin, P. J. Harvey, Yuen-Dat Chan, S. J. Brice, K. Graham, D. F. Cowen, C. E. Okada, J. D. Hepburn, R. G. H. Robertson, T. C. Andersen, Steven Elliott, J. J. Simpson, Peter Wittich, David A. Sinclair, E.D. Frank, A. S. Hamer, S. M. Oser, R. G. Stokstad, L. C. Stonehill, J. Maneira, R. G. Van de Water, I. Levine, N. Starinsky, P. M. Thornewell, T. J. Radcliffe, K. Frame, S. Majerus, J. H.M. Cowan, T. Spreitzer, D. L. Wark, J. Cameron, W. J. Heintzelman, Chris Waltham, C. J. Virtue, M. O'Neill, M. Moorhead, R. J. Komar, R. C. Allen, K. T. Lesko, M.G. Boulay, Joshua R. Klein, K. McFarlane, N. Gagnon, K. M. Heeger, I. T. Lawson, W. Frati, John L. Orrell, J. M. Wouters, Bhaskar Sur, B. C. Robertson, F. Dalnoki-Veress, H. B. Mak, Richard T. Kouzes, Q. R. Ahmad, A. P. Ferraris, R. J. Boardman, A. D. Marino, Anett Schulke, J. Bigu, M. Bercovitch, J. X. Wang, P. T. Keener, T. Kutter, R. Meijer Drees, G. A. Cox, V. L. Rusu, A. B. McDonald, R. S. Storey, G. McGregor, M. A. Howe, R. W. Ollerhead, A. J. Noble, H. Seifert, J. Manor, Y. I. Tserkovnyak, J. Lyon, Eric B. Norman, J. Heise, C. K. Hargrove, S. Luoma, M. Thorman, N. Tagg, J. F. Wilkerson, Reda Tafirout, Darren Grant, B. A. Moffat, J. G. Hykawy, W. F. Davidson, J. C. Barton, R. L. Helmer, I. Blevis, M. Omori, Monica Dunford, A. W. P. Poon, R. J. Ford, Xin Chen, P. Skensved, G. Milton, X. Dai, H. S. Ng, Mark Neubauer, M. G. Bowler, W. Locke, J. R. Leslie, J. Boger, B. T. Cleveland, W. B. Handler, M. Shatkay, M. W.E. Smith, Alan R. Smith, C. W. Nally, G. Bühler, C. Jillings, J. K. Rowley, C. A. Duba, G. G. Miller, Développement et Communication Chimique chez les Insectes ( DCCI ), Centre National de la Recherche Scientifique ( CNRS ) -Université de Bourgogne ( UB ) -AgroSup Dijon - Institut National Supérieur des Sciences Agronomiques, de l'Alimentation et de l'Environnement, and Delon, Viviane

Subjects
Particle physics, Physics::Instrumentation and Detectors, Solar neutrino, Astrophysics::High Energy Astrophysical Phenomena, General Physics and Astronomy, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), Tau neutrino, 0103 physical sciences, Nuclear Experiment (nucl-ex), 010306 general physics, Neutrino oscillation, Nuclear Experiment, Physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Solar neutrino problem, Neutrino detector, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Neutrino, Lepton
Abstract

Observations of neutral current neutrino interactions on deuterium in the Sudbury Neutrino Observatory are reported. Using the neutral current, elastic scattering, and charged current reactions and assuming the standard 8B shape, the electron-neutrino component of the 8B solar flux is 1.76 +/-0.05(stat.)+/-0.09(syst.) x10^6/(cm^2 s), for a kinetic energy threshold of 5 MeV. The non-electron neutrino component is 3.41+/-0.45(stat.)+0.48,-0.45(syst.) x10^6/(cm^2 s), 5.3 standard deviations greater than zero, providing strong evidence for solar electron neutrino flavor transformation. The total flux measured with the NC reaction is 5.09 +0.44,-0.43(stat.)+0.46,-0.43(syst.)x10^6/(cm^2 s), consistent with solar models., Comment: 6 pages, 3 figures, correction to author list and minor typographical corrections to references

Published
2002

31. Direct Evidence for Neutrino Flavor Transformation from Neutral-Current Interactions in SNO

Author

T. V. Bullard, M. H. Schwendener, B. C. Robertson, E. W. Beier, H. Fergani, G. Doucas, J. M. Wouters, H. W. Lee, J. Law, H. S. Ng, D. L. Wark, P. J. Doe, A. R. Smith, K. McFarlane, J. B. Wilhelmy, T. Kutter, Guthrie Miller, J.D. Anglin, A. S. Hamer, Q. R. Ahmad, C. J. Sims, J. V. Germani, M. Moorhead, R. Meijer Drees, J. Cameron, A. B. McDonald, H. Heron, F. Dalnoki-Veress, Min Chen, A. D. Marino, Christopher C. M. Kyba, John Heise, R. U. Haq, N. McCauley, K. Kazkaz, T. J. Radcliffe, R. G. H. Robertson, M. R. Dragowsky, E. Saettler, R. J. Boardman, T. Spreitzer, G. A. Cox, Andrew Hime, W. B. Handler, J.L. Hewett, Herbert H. Chen, Jochen Klein, Ilan Levine, C. J. Virtue, M. W.E. Smith, I. Lawson, N. Tagg, Anett Schulke, S. J. Brice, J. Bigu, Chris Waltham, A. J. Noble, Y. I. Tserkovnyak, R. L. Hahn, Salvador Gil, G. McGregor, J. G. Hykawy, Yuen-Dat Chan, A. P. Ferraris, J. X. Wang, E. D. Earle, A. L. Hallin, C. Mifflin, B. T. Cleveland, X. Chen, N.W. Tanner, K. Graham, L. C. Stonehill, S. M. Oser, J. Farine, Minfang Yeh, G. Jonkmans, N. West, V. L. Rusu, P. Skensved, M. Lay, R. K. Taplin, F. A. Duncan, J. H.M. Cowan, M. G. Boulay, W. J. Heintzelman, J. C. Barton, N. A. Jelley, M. Thorman, R. A. Black, M. O'Neill, J. J. Simpson, P. T. Keener, R. J. Ford, D. F. Cowen, Monica Dunford, J. Maneira, F. M. Newcomer, A. W. P. Poon, G. Bühler, J. A. Dunmore, A. Knox, P. T. Trent, R. W. Ollerhead, Peter Wittich, J. Lyon, M. C.P. Isaac, R. G. Stokstad, N. Gagnon, K. Frame, J. K. Rowley, B. A. Moffat, K. M. Heeger, I. Blevis, R. S. Storey, John L. Orrell, M. Omori, Joseph A. Formaggio, E. Bonvin, E. D. Hallman, R. Van Berg, W. Locke, A. Roberge, E. T.H. Clifford, J. Boger, T. J. Bowles, C. E. Okada, J. D. Hepburn, S. R. Elliott, David A. Sinclair, G. T. Ewan, T. D. Steiger, K. K. Schaffer, James R. Wilson, T. C. Andersen, A. A. Hamian, E.D. Frank, C. K. Hargrove, D. S. McDonald, X. Dai, V. M. Novikov, R. J. Komar, R. C. Allen, W. Frati, Bhaskar Sur, Mark Neubauer, Richard T. Kouzes, S. S.E. Rosendahl, Hal Evans, M. G. Bowler, M. C. Browne, Ryuta Hazama, R. L. Helmer, M. Bercovitch, S. Majerus, M. Shatkay, C. W. Nally, C. Jillings, C. A. Duba, H. B. Mak, W.F. Davidson, S. D. Biller, J. F. Wilkerson, Reda Tafirout, P. J. Harvey, Darren Grant, P. M. Thornewell, G. Milton, M. A. Howe, J. Manor, Malcolm M. Fowler, Eric B. Norman, H. Seifert, J. R. Leslie, P. Jagam, R. G. Van de Water, N. Starinsky, S. Luoma, and K. T. Lesko

Subjects
Physics, Particle physics, Sudbury Neutrino Observatory, Neutral current, Physics::Instrumentation and Detectors, Solar neutrino, Astrophysics::Cosmology and Extragalactic Astrophysics, Solar neutrino problem, Nuclear physics, Neutrino detector, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Neutrino, Nuclear Experiment, Neutrino oscillation, Charged current
Abstract

The Sudbury Neutrino Observatory (SNO) is a 1,000 tonne heavy water Cerenkov‐based neutrino detector situated 2,000 meters underground in INCO’s Creighton Mine near Sudbury, Ontario, Canada. For the neutrinos from 8B decay in the Sun SNO observes the Charged Current neutrino reaction sensitive only to electron neutrinos and others (Neutral Current and Elastic Scattering) sensitive to all active neutrino types and thereby can search for direct evidence of neutrino flavor change. Using these reactions and assuming the standard 8B shape, the ve component of the 8B solar flux is φe = 1.76−0.05+0.05(stat.)−0.09+0.09 (syst.) × 106 cm−2s−1 for a kinetic energy threshold of 5 MeV. The non‐ve component is φμτ = 3.41−0.45+0.45(stat.)−0.45+0.48 (syst.) × 106 cm−2s−1, 5.3σ greater than zero, providing strong evidence for solar ve flavor transformation. The total flux measured with the NC reaction is φNC = 5.09−0.43+0.44(stat.)−0.43+0.46 (syst.) × 106 cm−2s−1, consistent with solar models. For charged current events, ...

Published
2002
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32. Measurement of CC interactions produced by ${}^8$B solar neutrinos at SNO

Author

H. W. Lee, H. Mes, D. S. McDonald, John Heise, Ilan Levine, J. A. Dunmore, V. M. Novikov, R. U. Haq, Yuen-Dat Chan, J. F. Wilkerson, M. Moorhead, H. S. Ng, J. Cameron, Y. I. Tserkovnyak, Reda Tafirout, A. L. Hallin, E. T.H. Clifford, J. Boger, C. Mifflin, B. T. Cleveland, E. Bonvin, K. McFarlane, Darren Grant, N. Tagg, Christopher C. M. Kyba, C. E. Okada, J. D. Hepburn, S. M. Oser, David A. Sinclair, Hans C. Evans, T. V. Bullard, E. D. Earle, M. C.P. Isaac, R. W. Ollerhead, X. Chen, G. Milton, A. Roberge, N.W. Tanner, J. Lyon, Guthrie Miller, P. Skensved, H. B. Mak, I. Blevis, J. D. Anglin, E. D. Hallman, T. C. Andersen, E. W. Beier, J. H.M. Cowan, R. G. Stokstad, John L. Orrell, Q. R. Ahmad, F. M. Newcomer, C. J. Virtue, E. Saettler, E.D. Frank, Art Mc Donald, W.F. Davidson, Peter Wittich, P. J. Doe, P. Jagam, S. R. Elliott, M. Omori, Herbert H. Chen, G. T. Ewan, K. K. Schaffer, H. Heron, H. Fergani, J. Karn, Y. Dai, R. J. Ford, Klaus Kirch, D. L. Wark, B. A. Moffat, N. Starinsky, R. Heaton, F. A. Duncan, N. McCauley, C. K. Hargrove, J. C. Barton, B. C. Robertson, M. R. Dragowsky, R. K. Taplin, D. F. Cowen, M. G. Boulay, R. L. Hahn, Salvador Gil, F. Dalnoki-Veress, P. T. Trent, A. Goldschmidt, R. S. Storey, G. Doucas, A. S. Hamer, A. D. Marino, A. Knox, N. West, J. R. Leslie, S. D. Biller, R. J. Komar, R. C. Allen, M. W.E. Smith, M. Bercovitch, M. C. Chon, M. O'Neill, M. A. Howe, J. B. Wilhelmy, T. Kutter, R. Meijer Drees, Min Chen, P. J. Harvey, M. Lay, J. Bigu, S. J. Brice, G. McGregor, P. M. Thornewell, W. J. Heintzelman, R. J. Boardman, Richard George Van de Water, G. A. Cox, I. Lawson, T. J. Radcliffe, K. Frame, A. J. Noble, A. W. P. Poon, Malcolm M. Fowler, P. T. Keener, K. T. Lesko, J. J. Simpson, T. J. Bowles, K. M. Heeger, Eric B. Norman, G. Jonkmans, J. M. Wouters, H. Seifert, S. Luoma, A. Schuelke, Minfang Yeh, A. B. McDonald, N. A. Jelley, M. Thorman, A. P. Ferraris, J. X. Wang, V. L. Rusu, K. Cameron, J. G. Hykawy, J. Hewett, Andrew Hime, M. H. Schwendener, W. McLatchie, M. M. Lowry, J. Law, Jochen Klein, J. V. Germani, J. Farine, M. G. Bowler, M. C. Browne, T.H. Burritt, R. A. Black, G. Bühler, A. R. Smith, R. L. Helmer, W. Locke, J. K. Rowley, M. Shatkay, R. Van Berg, C. W. Nally, T. D. Steiger, A. A. Hamian, C. Jillings, Ryuta Hazama, Chris Waltham, S. Majerus, C. A. Duba, R. G. H. Robertson, W. Frati, Bhaskar Sur, Richard T. Kouzes, James R. Wilson, X. Dai, and Mark Neubauer

Subjects
Nuclear physics, Physics, Angular distribution, Solar neutrino, Neutrino oscillation, Charged current
Published
2001
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33. Measurement of the Rate ofνe+d→p+p+e−Interactions Produced byB8Solar Neutrinos at the Sudbury Neutrino Observatory

Author

G. Jonkmans, Y. Dai, J. M. Wouters, A. Goldschmidt, M. G. Bowler, J. Boger, M. Shatkay, John L. Orrell, R. G. Stokstad, C. W. Nally, P. Skensved, M. M. Fowler, J. C. Barton, X. Dai, M. C. Browne, Mark Neubauer, C. Jillings, C. A. Duba, B. C. Robertson, R. L. Helmer, Yuen-Dat Chan, P. Jagam, N. W. Tanner, A. L. Hallin, Chris Waltham, C. Mifflin, Steven Elliott, T. Kutter, J. B. Wilhelmy, H. W. Lee, R. Meijer Drees, R. K. Taplin, M. R. Dragowsky, S. M. Oser, K. Frame, R. U. Haq, N. McCauley, C. K. Hargrove, F.M. Newcomer, R. G. H. Robertson, J. D. Anglin, S. J. Brice, J. H.M. Cowan, C. J. Virtue, M. Moorhead, Peter Wittich, I. Blevis, T. C. Andersen, R. Heaton, S. Luoma, K. M. Heeger, F. A. Duncan, A. Schuelke, R. J. Ford, J. Cameron, M. Omori, R. S. Storey, M. A. Howe, Xin Chen, E.D. Frank, K. McFarlane, Minfang Yeh, N. A. Jelley, N. West, M. W.E. Smith, Q. R. Ahmad, Klaus Kirch, R. Van Berg, M. H. Schwendener, P. T. Trent, J. F. Wilkerson, Reda Tafirout, Mark Guy Boulay, Darren Grant, W. McLatchie, G. Milton, W. F. Davidson, J. Heise, J. G. Hykawy, H. Mes, E. T.H. Clifford, N. Tagg, H. S. Ng, J. Law, J. V. Germani, M. O'Neill, R. G. Van de Water, T. D. Steiger, N. Starinsky, R. J. Bardman, R. J. Komar, R. C. Allen, M. L. Chen, M. C. Chon, H. Seifert, J. Hewett, A. A. Hamian, Andrew Hime, J. Karn, I. T. Lawson, C. E. Okada, J. D. Hepburn, T. J. Bowles, W. Locke, J. R. Leslie, Eric B. Norman, David A. Sinclair, B. T. Cleveland, J. Bigu, G. McGregor, G. A. Cox, R. L. Hahn, Salvador Gil, K. Cameron, Alan R. Smith, J. R. Wilson, M. M. Lowry, H. Fergani, T.H. Burritt, J. A. Dunmore, G. Bühler, S. Majerus, S. D. Biller, Hal Evans, Joshua R. Klein, M. Lay, A. B. Knox, P. J. Harvey, D. S. McDonald, W. Frati, Bhaskar Sur, J. K. Rowley, A. S. Hamer, H. B. Mak, P. M. Thornewell, Richard T. Kouzes, J. J. Simpson, G. Doucas, V. M. Novikov, Y. I. Tserkovnyak, G. G. Miller, W. J. Heintzelman, E. D. Earle, P. T. Keener, K. T. Lesko, M. Thorman, J. Farine, M. C.P. Isaac, G. T. Ewan, K. K. Schaffer, R. A. Black, E. D. Hallman, E. Bonvin, A. B. McDonald, Christopher C. M. Kyba, R. Hazama, P. J. Doe, D. L. Wark, T. V. Bullard, A. Roberge, H. Heron, E. Saettler, E. W. Beier, F. Dalnoki-Veress, A. D. Marino, Herbert H. Chen, M. Bercovitch, D. F. Cowen, A. J. Noble, I. Levine, T. J. Radcliffe, A. W. P. Poon, A. P. Ferraris, J. X. Wang, V. L. Rusu, R. W. Ollerhead, J. Lyon, and B. A. Moffat

Subjects
Nuclear reaction, Physics, Particle physics, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Solar neutrino, General Physics and Astronomy, Flux, 01 natural sciences, 7. Clean energy, Nuclear physics, Massless particle, 13. Climate action, 0103 physical sciences, Neutrino, 010306 general physics, Charged current, Lepton
Abstract

Solar neutrinos from the decay of 8B have been detected at the Sudbury Neutrino Observatory (SNO) via the charged current (CC) reaction on deuterium and by the elastic scattering (ES) of electrons. The CC reaction is sensitive exclusively to νe, while the ES reaction also has a small sensitivity to νμ and ντ. The flux of νe from 8B decay measured by the CC reaction rate is φCC(ν e )=[1.75±0.07(stat.) −0.11 +0.12 (syst.)×0.05(theor.)]×106cm−2s−1. Assuming no flavor transformation, the flux inferred from the ES reaction rate is φES(ν x )=[2.39±0.34(stat.) −0.14 +0.16 (syst.)]×106cm−2s−1. Comparison of φCC(νe) to the Super-Kamiokande collaboration’s precision value of φES(νx) yields a 3.3σ difference, assuming the systematic uncertainties are normally distributed, providing evidence that there is a nonelectron flavor active neutrino component in the solar flux. The total flux of active 8B neutrinos is thus determined to be (5.44±0.99)×106 cm−2 s−1, in close agreement with the predictions of solar models.

Published
2001
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36. The Benefit of Fentanyl in Effective Sedation and Quality of Upper Endoscopy: A Double-Blinded Randomized Trial of Fentanyl Added to Midazolam Versus Midazolam Alone for Sedation.

Author

Khan KJ, Fergani H, Ganguli SC, Jalali S, Spaziani R, Tsoi K, and Morgan DG

Abstract

Aims: Our goals were to compare the effect of adding fentanyl to midazolam in a double-blinded, randomized, placebo-controlled trial and determine if fentanyl enhances sedation, increases adverse events or effects time of the procedure or discharge., Methods: Patients 18 to 65 years scheduled for outpatient upper endoscopy were eligible for the study. Patients were randomized to receive either 100 mcg/2 mL of Fentanyl or 2 mL of placebo IV with a double-blinded protocol. All patients received 2 mg of intravenous midazolam initially. Additional midazolam could be given to achieve adequate sedation., Results: There were 68 patients randomized to the Fentanyl group and 69 patients to the placebo group. The mean dose of midazolam was 4.0 mg for the Fentanyl group and 5.2 mg for placebo group ( P =0.003). Both endoscopist and nurse independently rated sedation to be better in the fentanyl group ( P =0001). The patient did not perceive any difference in sedation ( P =0.4). Procedure time was significantly shorter in the Fentanyl group (8.5 versus 11.1 minutes, P =0.001), with no difference in the discharge time. There was significantly less retching observed in patients in the fentanyl group ( P <0.001). There were no major complications., Conclusions: Endoscopists and nurses found adding fentanyl significantly improved sedation, led to a shorter procedure time, and allowed for less midazolam to be used per case. It did not affect the patient experience of sedation and was safe. Fentanyl use for routine outpatient upper endoscopy should be considered as a safe option to improve procedural sedation.NCT:01514695 (www.clinicaltrials.gov)Accepted as an abstract for the Canadian Digestive Diseases Week meeting in February 2014.

Published
2019
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37. 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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38. 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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39. 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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40. 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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41. 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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42. 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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