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1. Search for neutron-antineutron oscillations at the Sudbury Neutrino Observatory

Author

Aharmim, B, Ahmed, SN, Anthony, AE, Barros, N, Beier, EW, Bellerive, A, Beltran, B, Bergevin, M, Biller, SD, Boudjemline, K, Boulay, MG, Cai, B, Chan, YD, Chauhan, D, Chen, M, Cleveland, BT, Cox, GA, Dai, X, Deng, H, Detwiler, JA, Doe, PJ, Doucas, G, Drouin, P-L, Duncan, FA, Dunford, M, Earle, ED, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Fleurot, F, Ford, RJ, Formaggio, JA, Gagnon, N, Goon, JTM, Graham, K, Guillian, E, Habib, S, Hahn, RL, Hallin, AL, Hallman, ED, Harvey, PJ, Hazama, R, Heintzelman, WJ, Heise, J, Helmer, RL, Hime, A, Howard, C, Huang, M, Jagam, P, Jamieson, B, Jelley, NA, Jerkins, M, Keeter, KJ, Klein, JR, Kormos, LL, Kos, M, Kruger, A, Kraus, C, Krauss, CB, Kutter, T, Kyba, CCM, Lange, R, Law, J, Lawson, IT, Lesko, KT, Leslie, JR, Levine, I, Loach, JC, MacLellan, R, Majerus, S, Mak, HB, Maneira, J, Martin, RD, McCauley, N, McDonald, AB, McGee, SR, Miller, ML, Monreal, B, Monroe, J, Nickel, BG, Noble, AJ, O'Keeffe, HM, Oblath, NS, Okada, CE, Ollerhead, RW, Gann, GD Orebi, Oser, SM, Ott, RA, Peeters, SJM, Poon, AWP, Prior, G, Reitzner, SD, Rielage, K, Robertson, BC, Robertson, RGH, Schwendener, MH, Secrest, JA, Seibert, SR, Simard, O, Simpson, JJ, Sinclair, D, Skensved, P, Sonley, TJ, Stonehill, LC, Tesic, G, Tolich, N, Tsui, T, Van Berg, R, VanDevender, BA, Virtue, CJ, Wall, BL, Waller, D, Tseung, H Wan Chan, Wark, DL, Wendland, J, West, N, Wilkerson, JF, Wilson, JR, Wright, A, Yeh, M, Zhang, F, Zuber, K, and Collaboration, SNO

Subjects
Physics, Sudbury Neutrino Observatory, Particle physics, Physics - Instrumentation and Detectors, 010308 nuclear & particles physics, Physics beyond the Standard Model, Solar neutrino, FOS: Physical sciences, Instrumentation and Detectors (physics.ins-det), Solar neutrino problem, Antineutron, 01 natural sciences, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), Observatory, 0103 physical sciences, Neutron, Symmetry breaking, Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Experiment, QC
Abstract

Tests on $B-L$ symmetry breaking models are important probes to search for new physics. One proposed model with $\Delta(B-L)=2$ involves the oscillations of a neutron to an antineutron. In this paper a new limit on this process is derived for the data acquired from all three operational phases of the Sudbury Neutrino Observatory experiment. The search was concentrated in oscillations occurring within the deuteron, and 23 events are observed against a background expectation of 30.5 events. These translate to a lower limit on the nuclear lifetime of $1.48\times 10^{31}$ years at 90% confidence level (CL) when no restriction is placed on the signal likelihood space (unbounded). Alternatively, a lower limit on the nuclear lifetime was found to be $1.18\times 10^{31}$ years at 90% CL when the signal was forced into a positive likelihood space (bounded). Values for the free oscillation time derived from various models are also provided in this article. This is the first search for neutron-antineutron oscillation with the deuteron as a target., Comment: 14 pages, 8 figures

Published
2017

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

Author

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

Published
2007

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

Author

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

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

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

Published
2005

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

Author

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

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

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

Published
2005

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

Author

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

Published
2005

6. The Sudbury Neutrino Observatory

Author

Boger, J, Hahn, RL, Rowley, JK, Carter, AL, Hollebone, B, Kessler, D, Blevis, I, Dalnoki-Veress, F, DeKok, A, Farine, J, Grant, DR, Hargrove, CK, Laberge, G, Levine, I, McFarlane, K, Mes, H, Noble, AT, Novikov, VM, O'Neill, M, Shatkay, M, Shewchuk, C, Sinclair, D, Clifford, ETH, Deal, R, Earle, ED, Gaudette, E, Milton, G, Sur, B, Bigu, J, Cowan, JHM, Cluff, DL, Hallman, ED, Haq, RU, Hewett, J, Hykawy, JG, Jonkmans, G, Michaud, R, Roberge, A, Roberts, J, Saettler, E, Schwendener, MH, Seifert, H, Sweezey, D, Tafirout, R, Virtue, CJ, Beck, DN, Chan, YD, Chen, X, Dragowsky, MR, Dycus, FW, Gonzalez, J, Isaac, MCP, Kajiyama, Y, Koehler, GW, Lesko, KT, Moebus, MC, Norman, EB, Okada, CE, Poon, AWP, Purgalis, P, Schuelke, A, Smith, AR, Stokstad, RG, Turner, S, Zlimen, I, Anaya, JM, Bowles, TJ, Brice, SJ, Esch, EI, Fowler, MM, Goldschmidt, A, Hime, A, McGirt, AF, Miller, GG, Teasdale, WA, Wilhelmy, JB, Wouters, JM, Anglin, JD, Bercovitch, M, Davidson, WF, Storey, RS, Biller, S, Black, RA, Boardman, RJ, Bowler, MG, Cameron, J, Cleveland, B, Ferraris, AP, Doucas, G, Heron, H, Howard, C, Jelley, NA, Knox, AB, Lay, M, Locke, W, Lyon, J, Majerus, S, Moorhead, M, Omori, M, Tanner, NW, Taplin, RK, Thorman, M, Wark, DL, West, N, Barton, JC, Trent, PT, Kouzes, R, Lowry, MM, Bell, AL, Bonvin, E, Boulay, M, Dayon, M, Duncan, F, Erhardt, LS, Evans, HC, Ewan, GT, Ford, R, Hallin, A, Hamer, A, Hart, PM, Harvey, PJ, Haslip, D, Hearns, CAW, Heaton, R, Hepburn, JD, Jillings, CJ, Korpach, EP, Lee, HW, Leslie, JR, Liu, MQ, Mak, HB, McDonald, AB, MacArthur, JD, McLatchie, W, Moffat, BA, Noel, S, Radcliffe, TJ, Robertson, BC, Skensved, P, Stevenson, RL, Zhu, X, Gil, S, Heise, J, Helmer, RL, Komar, RJ, Nally, CW, Ng, HS, Waltham, CE, Allen, RC, Buhler, G, Chen, HH, Aardsma, G, Andersen, T, Cameron, K, Chon, MC, Hanson, RH, Jagam, P, Karn, J, Law, J, Ollerhead, RW, Simpson, JJ, Tagg, N, Wang, JX, Alexander, C, Beier, EW, Cook, JC, Cowen, DF, Frank, ED, Frati, W, Keener, PT, Klein, JR, Mayers, G, McDonald, DS, Neubauer, MS, Newcomer, FM, Pearce, RJ, Van de Water, RG, Van Berg, R, Wittich, P, Ahmad, QR, Beck, JM, Browne, MC, Burritt, TH, Doe, PJ, Duba, CA, Elliott, SR, Franklin, JE, Germani, JV, Green, P, Hamian, AA, Heeger, KM, Howe, M, Drees, RM, Myers, A, Robertson, RGH, Smith, MWE, Steiger, TD, Van Wechel, T, Wilkerson, JF, and Collaboration, SNO

Subjects
Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, 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), High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Nuclear Experiment (nucl-ex), Nuclear Experiment, 010306 general physics, Neutrino oscillation, Instrumentation, Physics, Standard solar model, Sudbury Neutrino Observatory, 010308 nuclear & particles physics, Astrophysics (astro-ph), High Energy Physics::Phenomenology, Instrumentation and Detectors (physics.ins-det), High Energy Physics - Phenomenology, Neutrino detector, High Energy Physics::Experiment, Neutrino, Electron neutrino, Lepton
Abstract

The Sudbury Neutrino Observatory is a second generation water Cherenkov detector designed to determine whether the currently observed solar neutrino deficit is a result of neutrino oscillations. The detector is unique in its use of D2O as a detection medium, permitting it to make a solar model-independent test of the neutrino oscillation hypothesis by comparison of the charged- and neutral-current interaction rates. In this paper the physical properties, construction, and preliminary operation of the Sudbury Neutrino Observatory are described. Data and predicted operating parameters are provided whenever possible., 58 pages, 12 figures, submitted to Nucl. Inst. Meth. Uses elsart and epsf style files. For additional information about SNO see http://www.sno.phy.queensu.ca . This version has some new references

Published
2000

7. Measuring Concentrations of Particulate 140La in the Air.

Author

Okada CE, Kernan W, Keillor M, Kirkham R, Sorom RD, and Van Etten DM

Subjects
Humans, Radiation Protection, Air Pollutants, Radioactive analysis, Lanthanum analysis, Particulate Matter analysis, Radiation Monitoring
Abstract

Air sampling systems were deployed to measure the concentration of radioactive material in the air during the Full-Scale Radiological Dispersal Device Field Trials. The air samplers were positioned 100-600 m downwind of the release point. The filters were collected immediately and analyzed in a field laboratory. Quantities for total activity collected on the air filters are reported along with additional information to compute the average or integrated air concentrations.

Published
2016
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8. Enhanced analysis methods to derive the spatial distribution of 131I deposition on the ground by airborne surveys at an early stage after the Fukushima Daiichi nuclear power plant accident.

Author

Torii T, Sugita T, Okada CE, Reed MS, and Blumenthal DJ

Subjects
Cesium Radioisotopes analysis, Iodine Radioisotopes analysis, Spatial Analysis, Time Factors, Air analysis, Data Collection, Fukushima Nuclear Accident, Nuclear Power Plants, Radiation Monitoring methods, Radioactive Fallout analysis
Abstract

This paper applies both new and well tested analysis methods to aerial radiological surveys to extract the I ground concentrations present after the March 2011 Fukushima Daiichi nuclear power plant (NPP) accident. The analysis provides a complete map of I deposition, an important quantity incalculable at the time of the accident due to the short half-life of I and the complexity of the analysis. A map of I deposition is the first step in conducting internal exposure assessments, population dose reconstruction, and follow-up epidemiological studies. The short half-life of I necessitates the use of aerial radiological surveys to cover the large area quickly, thoroughly, and safely. Teams from the U.S. Department of Energy National Nuclear Security Administration (DOE/NNSA) performed aerial radiological surveys to provide initial maps of the dispersal of radioactive material in Japan. This work reports on analyses performed on a subset of the initial survey data by a joint Japan-U.S. collaboration to determine I ground concentrations. The analytical results show a high concentration of I northwest of the NPP, consistent with the previously reported radioactive cesium deposition, but also shows a significant I concentration south of the plant, which was not observed in the original cesium analysis. The difference in the radioactive iodine and cesium patterns is possibly the result of differences in the ways these materials settle out of the air.

Published
2013
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9. 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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10. 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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11. High sensitivity search for nu;e's from the sun and other sources at KamLAND.

Author

Eguchi K, Enomoto S, Furuno K, Ikeda H, Ikeda K, Inoue K, Ishihara K, Iwamoto T, Kawashima T, Kishimoto Y, Koga M, Koseki Y, Maeda T, Mitsui T, Motoki M, Nakajima K, Ogawa H, Owada K, Piquemal F, Shimizu I, Shirai J, Suekane F, Suzuki A, Tada K, Tajima O, Takayama T, Tamae K, Watanabe H, Busenitz J, Djurcic Z, McKinny K, Mei DM, Piepke A, Yakushev E, Berger BE, Chan YD, Decowski MP, Dwyer DA, Freedman SJ, Fu Y, Fujikawa BK, Goldman J, Heeger KM, Lesko KT, Luk KB, Murayama H, Nygren DR, Okada CE, Poon AW, Steiner HM, Winslow LA, Horton-Smith GA, Mauger C, McKeown RD, Tipton B, Vogel P, Lane CE, Miletic T, Gorham PW, Guillian G, Learned JG, Maricic J, Matsuno S, Pakvasa S, Dazeley S, Hatakeyama S, Svoboda R, Dieterle BD, DiMauro M, Detwiler J, Gratta G, Ishii K, Tolich N, Uchida Y, Batygov M, Bugg W, Efremenko Y, Kamyshkov Y, Kozlov A, Nakamura Y, Gould CR, Karwowski HJ, Markoff DM, Messimore JA, Nakamura K, Rohm RM, Tornow W, Young AR, Chen MJ, and Wang YF

Abstract

Data corresponding to a KamLAND detector exposure of 0.28 kton yr has been used to search for nu;(e)'s in the energy range 8.3

Published
2004
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12. First results from KamLAND: evidence for reactor antineutrino disappearance.

Author

Eguchi K, Enomoto S, Furuno K, Goldman J, Hanada H, Ikeda H, Ikeda K, Inoue K, Ishihara K, Itoh W, Iwamoto T, Kawaguchi T, Kawashima T, Kinoshita H, Kishimoto Y, Koga M, Koseki Y, Maeda T, Mitsui T, Motoki M, Nakajima K, Nakajima M, Nakajima T, Ogawa H, Owada K, Sakabe T, Shimizu I, Shirai J, Suekane F, Suzuki A, Tada K, Tajima O, Takayama T, Tamae K, Watanabe H, Busenitz J, Djurcic Z, McKinny K, Mei DM, Piepke A, Yakushev E, Berger BE, Chan YD, Decowski MP, Dwyer DA, Freedman SJ, Fu Y, Fujikawa BK, Heeger KM, Lesko KT, Luk KB, Murayama H, Nygren DR, Okada CE, Poon AW, Steiner HM, Winslow LA, Horton-Smith GA, McKeown RD, Ritter J, Tipton B, Vogel P, Lane CE, Miletic T, Gorham PW, Guillian G, Learned JG, Maricic J, Matsuno S, Pakvasa S, Dazeley S, Hatakeyama S, Murakami M, Svoboda RC, Dieterle BD, DiMauro M, Detwiler J, Gratta G, Ishii K, Tolich N, Uchida Y, Batygov M, Bugg W, Cohn H, Efremenko Y, Kamyshkov Y, Kozlov A, Nakamura Y, De Braeckeleer L, Gould CR, Karwowski HJ, Markoff DM, Messimore JA, Nakamura K, Rohm RM, Tornow W, Young AR, and Wang YF

Abstract

KamLAND has measured the flux of nu;(e)'s from distant nuclear reactors. We find fewer nu;(e) events than expected from standard assumptions about nu;(e) propagation at the 99.95% C.L. In a 162 ton.yr exposure the ratio of the observed inverse beta-decay events to the expected number without nu;(e) disappearance is 0.611+/-0.085(stat)+/-0.041(syst) for nu;(e) energies >3.4 MeV. In the context of two-flavor neutrino oscillations with CPT invariance, all solutions to the solar neutrino problem except for the "large mixing angle" region are excluded.

Published
2003
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13. 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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14. 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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15. 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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