High sensitivity characterization of an ultrahigh purity NaI(Tl) crystal scintillator with the SABRE proof-of-principle detector
High sensitivity characterization of an ultrahigh purity NaI(Tl) crystal scintillator with the SABRE proof-of-principle detector
复制标题
使用 SABRE 原理验证探测器对超高纯度 NaI(Tl) 晶体闪烁体进行高灵敏度表征
DOI：
10.1103/physrevd.104.l021302
复制
发表时间：
2021
影响因子：
5
通讯作者：
Ianni, A.
中科院分区：
文献类型：
--
作者：
Calaprice, F.;Copello, S.;Dafinei, I.;D’Angelo, D.;D’Imperio, G.;Di Carlo, G.;Diemoz, M.;Di Giacinto, A.;Di Ludovico, A.;Ianni, A.
我们提出了一个3.4公斤的碘化钠（铊）晶体闪烁体在SABRE的原理验证探测器设置操作的放射性纯度的新结果。通过放射性直接计数确定的钾污染量是NaI（Tl）晶体有史以来最低的。在主动否决下，晶体中1-6 keV能量感兴趣区（ROI）的平均本底率为，这是自DAMA/LIBRA实验以来的突破。我们的背景模型表明，该速率是由，约一半的这种污染位于聚四氟乙烯反射器。我们讨论了晶体制造的持续发展，旨在进一步减少背景，包括通过区域精炼纯化的数据。一个低于投资回报率的预计背景率是可以达到的。这些结果代表了下一代NaI（Tl）探测器阵列直接探测暗物质粒子的发展基准。
We present new results on the radiopurity of a 3.4-kg NaI(Tl) crystal scintillator operated in the SABRE proof-of-principle detector setup. The amount of potassium contamination, determined by the direct counting of radioactive, is found to be, lowest ever achieved for NaI(Tl) crystals. With the active veto, the average background rate in the crystal in the 1–6 keV energy region of interest (ROI) is, which is a breakthrough since the DAMA/LIBRA experiment. Our background model indicates that the rate is dominated byand that about half of this contamination is located in the polytetrafluoroethylene reflector. We discuss ongoing developments of the crystal manufacture aimed at the further reduction of the background, including data from purification by zone refining. A projected background rate lower thanin the ROI is within reach. These results represent a benchmark for the development of next-generation NaI(Tl) detector arrays for the direct detection of dark matter particles.
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低本底探测器用超高纯碘化钠的区域精炼
影响因子：
4.6
作者：
Suerfu, Burkhant;Calaprice, Frank;Souza, Michael
通讯作者：
Souza, Michael
坎弗兰克地下实验室：一个多学科的地下设施
DOI：
--
发表时间：
2016
期刊：
影响因子：
--
作者：
A. Ianni
通讯作者：
A. Ianni
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.
使用超低背景大表面 α 光谱仪研究金属中的表面和本体 210Po。
影响因子：
1.6
作者：
G. Zuzel;K. Pelczar;M. Wójcik
通讯作者：
M. Wójcik