The SABRE experiment
The SABRE experiment
复制标题
军刀实验
DOI：
10.1142/s0217751x22400164
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发表时间：
2022
影响因子：
1.6
通讯作者：
Tomei, C.
中科院分区：
文献类型：
--
作者：
Zani, A.;D’Angelo, D.;Vignoli, C.;Di Carlo, G.;Di Giacinto, A.;Ianni, A.;Orlandi, D.;Mariani, A.;Copello, S.;Tomei, C.
DAMA/LIBRA年度调制信号的暗物质解释是天体粒子物理学中一个长期存在的悬而未决的问题。SABRE实验旨在验证这种说法，将相同的检测技术提高到前所未有的灵敏度。SABRE基于超低本底NaI（Tl）闪烁晶体（如DAMA），其特点是围绕主目标的液体闪烁体Veto系统，它将部署两个探测器：一个在北方半球的意大利Gran Sasso国家实验室（LNGS），另一个在澳大利亚的斯塔韦尔地下物理实验室（SUPL），这是南半球的第一个此类实验室。该合作生产的第一个极高纯度晶体于2019年运往LNGS进行表征。它的特点是钾污染，通过质谱测量，约为4 ppb，比DAMA/LIBRA晶体低三倍。SABRE实验的第一阶段是LNGS的原理验证（PoP）探测器，具有一个晶体和一个液体闪烁体Veto。本文将介绍第一颗SABRE高纯度晶体的独立表征结果，以及2020年夏初投入使用的PoP探测器的状态。
The dark matter interpretation of the DAMA/LIBRA annual modulation signal represents a long-standing open question in astroparticle physics. The SABRE experiment aims to test such claim, bringing the same detection technique to an unprecedented sensitivity. Based on ultra-low background NaI(Tl) scintillating crystals like DAMA, SABRE features a liquid scintillator Veto system, surrounding the main target, and it will deploy twin detectors: one in the Northern hemisphere at Laboratori Nazionali del Gran Sasso (LNGS), Italy and the other in the Stawell Underground Physics Laboratory (SUPL), Australia, first laboratory of this kind in the Southern hemisphere. The first very-high-purity crystal produced by the collaboration was shipped to LNGS in 2019 for characterization. It features a potassium contamination, measured by mass spectroscopy, of the order of 4 ppb, about three times lower than DAMA/LIBRA crystals. The first phase of the SABRE experiment is a Proof-of-Principle (PoP) detector featuring one crystal and a liquid scintillator Veto, at LNGS. This contribution will present the results of the stand-alone characterization of the first SABRE high-purity crystal, as well as the status of the PoP detector, commissioned early in the summer of 2020.
影响因子：
3.5
作者：
M. Antonello;E. Barberio;T. Baroncelli;J. Benziger;L. Bignell;I. Bolognino;F. Calaprice;S. Copello;D. D’Angelo;G. D’Imperio;I. Dafinei;G. D. Carlo;M. Diemoz;A. D. Ludovico;A. Duffy;F. Froborg;G. Giovanetti;E. Hoppe;A. Ianni;L. Ioannucci;S. Krishnan;G. Lane;I. Mahmood;A. Mariani;P. McGee;P. Montini;J. Mould;F. Nuti;D. Orlandi;M. Paris;V. Pettinacci;L. Pietrofaccia;D. Prokopovich;S. Rahatlou;N. Rossi;A. Sarbutt;E. Shields;M. Souza;A. Stuchbery;B. Suerfu;C. Tomei;P. Urquijo;C. Vignoli;M. Wada;A. Wallner;A. G. Williams;J. Xu;M. Milano;Milano;Italy;S. O. Physics;The University of Melbourne;Melbourne;Australia;Chemical Engineering Department;Princeton University;Princeton;Nj;USA.;D. Physics;The Australian National University;Canberra;D. Fisica;U. D. S. D. Milano-U.-D.-S.-D.-Milano-102421132;P. Department;I. G. Sasso;Assergi;I. -. G. S. S. Institute-I.-.-G.-S.-S.-Institute-102945001;Infn Roma;Roma;A. J. W. H. C. F. Astrophysics;Centre for Gravitational Astrophysics;Supercomputing;S. U. Technology;I. -. London;High Energy Physics;B. Laboratory;United Kingdom.;P. N. N. Laboratory-P.-N.-N.-Laboratory-7290024;Richland;Wa;The University of Adelaide;Adelaide;South Australia.;S. Roma;Australian Nuclear Science;Technology Organization;Lucas Heights
通讯作者：
M. Antonello;E. Barberio;T. Baroncelli;J. Benziger;L. Bignell;I. Bolognino;F. Calaprice;S. Copello;D. D’Angelo;G. D’Imperio;I. Dafinei;G. D. Carlo;M. Diemoz;A. D. Ludovico;A. Duffy;F. Froborg;G. Giovanetti;E. Hoppe;A. Ianni;L. Ioannucci;S. Krishnan;G. Lane;I. Mahmood;A. Mariani;P. McGee;P. Montini;J. Mould;F. Nuti;D. Orlandi;M. Paris;V. Pettinacci;L. Pietrofaccia;D. Prokopovich;S. Rahatlou;N. Rossi;A. Sarbutt;E. Shields;M. Souza;A. Stuchbery;B. Suerfu;C. Tomei;P. Urquijo;C. Vignoli;M. Wada;A. Wallner;A. G. Williams;J. Xu;M. Milano;Milano;Italy;S. O. Physics;The University of Melbourne;Melbourne;Australia;Chemical Engineering Department;Princeton University;Princeton;Nj;USA.;D. Physics;The Australian National University;Canberra;D. Fisica;U. D. S. D. Milano-U.-D.-S.-D.-Milano-102421132;P. Department;I. G. Sasso;Assergi;I. -. G. S. S. Institute-I.-.-G.-S.-S.-Institute-102945001;Infn Roma;Roma;A. J. W. H. C. F. Astrophysics;Centre for Gravitational Astrophysics;Supercomputing;S. U. Technology;I. -. London;High Energy Physics;B. Laboratory;United Kingdom.;P. N. N. Laboratory-P.-N.-N.-Laboratory-7290024;Richland;Wa;The University of Adelaide;Adelaide;South Australia.;S. Roma;Australian Nuclear Science;Technology Organization;Lucas Heights
通过直接地下计数表征 SABRE 晶体 NaI-33
DOI：
10.1140/epjc/s10052-021-09098-5
发表时间：
2021
期刊：
The European Physical Journal C
影响因子：
--
作者：
Antonello, M.;Arnquist, I. J.;Barberio, E.;Baroncelli, T.;Benziger, J.;Bignell, L. J.;Bolognino, I.;Calaprice, F.;Copello, S.;Dafinei, I.
通讯作者：
Dafinei, I.