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物理学 > 仪器与探测器

arXiv:1508.05759v3 (physics)
[提交于 2015年8月24日 (v1) ,最后修订 2016年1月28日 (此版本, v3)]

标题: SNO+实验的现状与未来前景

标题: Current Status and Future Prospects of the SNO+ Experiment

Authors:SNO+ Collaboration: S. Andringa (1), E. Arushanova (2), S. Asahi (3), M. Askins (4), D. J. Auty (5), A. R. Back (2,6), Z. Barnard (7), N. Barros (1,8), E. W. Beier (8), A. Bialek (5), S. D. Biller (9), E. Blucher (10), R. Bonventre (8), D. Braid (7), E. Caden (7), E. Callaghan (8), J. Caravaca (11,12), J. Carvalho (13), L. Cavalli (9), D. Chauhan (1,3,7), M. Chen (3), O. Chkvorets (7), K. Clark (3,6,9), B. Cleveland (7,14), I. T. Coulter (8,9), D. Cressy (7), X. Dai (3), C. Darrach (7), B. Davis-Purcell (15), R. Deen (8,9), M. M. Depatie (7), F. Descamps (11,12), F. Di Lodovico (2), N. Duhaime (7), F. Duncan (7,14), J. Dunger (9), E. Falk (6), N. Fatemighomi (3), R. Ford (7,14), P. Gorel (5), C. Grant (4), S. Grullon (8), E. Guillian (3), A. L. Hallin (5), D. Hallman (7), S. Hans (16), J. Hartnell (6), P. Harvey (3), M. Hedayatipour (5), W. J. Heintzelman (8), R. L. Helmer (15), B. Hreljac (7), J. Hu (5), T. Iida (3), C. M. Jackson (11,12), N. A. Jelley (9), C. Jillings (7,14), C. Jones (9), P. G. Jones (2,9), K. Kamdin (11,12), T. Kaptanoglu (8), J. Kaspar (17), P. Keener (8), P. Khaghani (7), L. Kippenbrock (17), J. R. Klein (8), R. Knapik (8,18), J. N. Kofron (17), L. L. Kormos (19), S. Korte (7), C. Kraus (7), C. B. Krauss (5), K. Labe (10), I. Lam (3), C. Lan (3), B. J. Land (11,12), S. Langrock (2), A. LaTorre (10), I. Lawson (7,14), G. M. Lefeuvre (6), E. J. Leming (6), J. Lidgard (9), X. Liu (3), Y. Liu (3), V. Lozza (20), S. Maguire (16), A. Maio (1,21), K. Majumdar (9), S. Manecki (3), J. Maneira (1,21), E. Marzec (8), A. Mastbaum (8), N. McCauley (22), A. B. McDonald (3), J. E. McMillan (23), P. Mekarski (5), C. Miller (3), Y. Mohan (8), E. Mony
(3), M. J. Mottram (2,6), V. Novikov (3), H. M. O'Keeffe (3,19), E. O'Sullivan (3), G. D. Orebi Gann (8,11,12), M. J. Parnell (19), S. J. M. Peeters (6), T. Pershing (4), Z. Petriw (5), G. Prior (1), J. C. Prouty (11,12), S. Quirk (3), A. Reichold (9), A. Robertson (22), J. Rose (22), R. Rosero (16), P. M. Rost (7), J. Rumleskie (7), M. A. Schumaker (7), M. H. Schwendener (7), D. Scislowski (17), J. Secrest (24), M. Seddighin (3), L. Segui (9), S. Seibert (8), T. Shantz (7), T. M. Shokair (8), L. Sibley (5), J. R. Sinclair (6), K. Singh (5), P. Skensved (3), A. Soerensen (20), T. Sonley (3), R. Stainforth (22), M. Strait (10), M. I. Stringer (6), R. Svoboda (4), J. Tatar (17), L. Tian (3), N. Tolich (17), J. Tseng (9), H. W. C. Tseung (17), R. Van Berg (8), E. Vázquez-Jáuregui (14,25), C. Virtue (7), B. von Krosigk (20), J. M. G. Walker (22), M. Walker (3), O. Wasalski (15), J. Waterfield (6), R. F. White (6), J. R. Wilson (2), T. J. Winchester (17), A. Wright (3), M. Yeh (16), T. Zhao (3), K. Zuber (20) ((1) Laboratório de Instrumentaçao e Física Experimental de Partículas (LIP), Lisboa, Portugal, (2) Queen Mary, University of London, School of Physics and Astronomy, London, UK, (3) Queen's University, Department of Physics, Engineering Physics and Astronomy, Kingston, ON, Canada, (4) University of California, Davis, CA, USA, (5) University of Alberta, Department of Physics, Edmonton, AB, Canada, (6) University of Sussex, Physics and Astronomy, Falmer, Brighton, UK, (7) Laurentian University, Sudbury, ON, Canada, (8) University of Pennsylvania, Department of Physics and Astronomy, Philadelphia, PA, USA, (9) University of Oxford, The Denys Wilkinson Building, Oxford, UK, (10) The Enrico Fermi Institute and Department of Physics, The University of Chicago, Chicago, IL, USA, (11) University of California, Department of Physics, Berkeley, CA, USA, (12) Lawrence Berkeley National Laboratory, Nuclear Science Division, CA, USA, (13) Universidade de Coimbra, Laboratório de Instrumentaçao e Física Experimental de Partículas and Departamento de Física, Coimbra, Portugal, (14) SNOLAB, Sudbury, ON, Canada, (15) TRIUMF, Vancouver, BC, Canada, (16) Brookhaven National Laboratory, Chemistry Department, Upton, NY, USA, (17) University of Washington, Center for Experimental Nuclear Physics and Astrophysics, and Department of Physics, Seattle, WA, USA, (18) Norwich University, Northfield, VT, USA, (19) Lancaster University, Physics Department, Lancaster, UK, (20) Technische Universität Dresden, Institut für Kern- und Teilchenphysik, Dresden, Germany, (21) Universidade de Lisboa, Departamento de Física, Faculdade de Ciências, Lisboa, Portugal, (22) University of Liverpool, Department of Physics, Liverpool, UK, (23) University of Sheffield, Department of Physics and Astronomy, Sheffield, UK, (24) Armstrong Atlantic State University, Savannah, GA, USA, (25) Universidad Nacional Autónoma de México (UNAM), Instituto de Física, México D.F., México)
et al. (57 additional authors not shown)
摘要: SNO+是一个位于加拿大苏德伯里SNOLAB地下2公里处的大型液体闪烁体实验。 它重新使用了苏德伯里中微子观测站探测器,由一个直径12米的亚克力容器组成,该容器将装入约780吨超纯液体闪烁体。 设计为多用途中微子实验,SNO+的主要目标是寻找130Te的无中微子双β衰变(0$\nu\beta\beta$)。 在第一阶段,探测器将装载0.3%的天然碲,相当于近800千克的130Te,在倒置质量顺序区域预计有效马约拉纳中微子质量灵敏度为 55-133 meV,略高于倒置质量顺序。 最近,已经研究了部署多达十倍于天然碲的可能性,这将使SNO+在未来能够深入倒置中微子质量顺序的参数空间。 此外,SNO+旨在测量反应堆反中微子振荡、低能太阳中微子和地中微子,对超新星中微子敏感,并寻找奇异物理现象。 探测器装满水的第一阶段即将开始,预计在几个月的水数据采集之后开始闪烁体阶段。 0$\nu\beta\beta$第一阶段预计在2017年进行。
摘要: SNO+ is a large liquid scintillator-based experiment located 2km underground at SNOLAB, Sudbury, Canada. It reuses the Sudbury Neutrino Observatory detector, consisting of a 12m diameter acrylic vessel which will be filled with about 780 tonnes of ultra-pure liquid scintillator. Designed as a multipurpose neutrino experiment, the primary goal of SNO+ is a search for the neutrinoless double-beta decay (0$\nu\beta\beta$) of 130Te. In Phase I, the detector will be loaded with 0.3% natural tellurium, corresponding to nearly 800 kg of 130Te, with an expected effective Majorana neutrino mass sensitivity in the region of 55-133 meV, just above the inverted mass hierarchy. Recently, the possibility of deploying up to ten times more natural tellurium has been investigated, which would enable SNO+ to achieve sensitivity deep into the parameter space for the inverted neutrino mass hierarchy in the future. Additionally, SNO+ aims to measure reactor antineutrino oscillations, low-energy solar neutrinos, and geoneutrinos, to be sensitive to supernova neutrinos, and to search for exotic physics. A first phase with the detector filled with water will begin soon, with the scintillator phase expected to start after a few months of water data taking. The 0$\nu\beta\beta$ Phase I is foreseen for 2017.
评论: 发表于《中微子质量与振荡》(《高能物理进展》, Hindawi)
主题: 仪器与探测器 (physics.ins-det) ; 高能物理 - 实验 (hep-ex)
引用方式: arXiv:1508.05759 [physics.ins-det]
  (或者 arXiv:1508.05759v3 [physics.ins-det] 对于此版本)
  https://doi.org/10.48550/arXiv.1508.05759
通过 DataCite 发表的 arXiv DOI
期刊参考: Advances in High Energy Physics, vol. 2016, 6194250
相关 DOI: https://doi.org/10.1155/2016/6194250
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来自: Valentina Lozza Ph.D. [查看电子邮件]
[v1] 星期一, 2015 年 8 月 24 日 11:13:36 UTC (651 KB)
[v2] 星期五, 2015 年 11 月 13 日 10:46:04 UTC (652 KB)
[v3] 星期四, 2016 年 1 月 28 日 13:55:11 UTC (652 KB)
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