Characterization of SABRE crystal NaI-33 with direct underground counting
Characterization of SABRE crystal NaI-33 with direct underground counting
复制标题
通过直接地下计数表征 SABRE 晶体 NaI-33
DOI：
10.1140/epjc/s10052-021-09098-5
复制
发表时间：
2021
期刊：
影响因子：
--
通讯作者：
Dafinei, I.
中科院分区：
文献类型：
--
作者：
Antonello, M.;Arnquist, I. J.;Barberio, E.;Baroncelli, T.;Benziger, J.;Bignell, L. J.;Bolognino, I.;Calaprice, F.;Copello, S.;Dafinei, I.
超纯NaI（Tl）晶体是DAMA结果的模型独立验证的关键元素，也是寻找暗物质相互作用的年度调制特征的有力手段。多年来，SABRE合作一直在开发减少固有背景的尖端技术。在本文中，我们报告的第一个表征的3.4公斤的晶体，命名为碘化钠-33，在地下被动屏蔽设置在LNGS。NaI-33具有4.3 ± 0.2 ppb的创纪录低K污染，如通过质谱测定的。在59.5 keV处，我们测得光产额为11.1 ± 0.2个光电子/keV，能量分辨率为13.2%（FWHM/E）。我们估算出晶体中Ra和Th的活度分别为Bq/kg和Bq/kg，这表明铀和钍的污染程度为万亿分之一。在5304 keV处测得铅的失平衡活度为0.51 ± 0.02mBq/kg，猝灭因子为0.63 ± 0.01。我们说明了分析技术，拒绝电子噪声的能量谱的较低部分。基于切割的策略和多变量方法表明，在[5-20] keV区域，归因于晶体固有放射性的速率为1计数/天/kg/keV。
Ultra-pure NaI(Tl) crystals are the key element for a model-independent verification of the long standing DAMA result and a powerful means to search for the annual modulation signature of dark matter interactions. The SABRE collaboration has been developing cutting-edge techniques for the reduction of intrinsic backgrounds over several years. In this paper we report the first characterization of a 3.4 kg crystal, named NaI-33, performed in an underground passive shielding setup at LNGS. NaI-33 has a record lowK contamination of 4.3 ± 0.2 ppb as determined by mass spectrometry. We measured a light yield of 11.1 ± 0.2 photoelectrons/keV and an energy resolution of 13.2% (FWHM/E) at 59.5 keV. We evaluated the activities ofRa andTh inside the crystal to beBq/kg andBq/kg, respectively, which would indicate a contamination fromU andTh at part-per-trillion level. We measured an activity of 0.51 ± 0.02 mBq/kg due toPb out of equilibrium and aquenching factor of 0.63 ± 0.01 at 5304 keV. We illustrate the analyses techniques developed to reject electronic noise in the lower part of the energy spectrum. A cut-based strategy and a multivariate approach indicated a rate, attributed to the intrinsic radioactivity of the crystal, of1 count/day/kg/keV in the [5–20] keV region.
登录
查看更多内容
影响因子：
3.5
作者：
de Souza, E. Barbosa;Park, B. J.;Yu, G. H.
通讯作者：
Yu, G. H.
影响因子：
5
作者：
R. Agnese;A. Anderson;T. Aralis;T. Aramaki;I. Arnquist;W. Baker;D. Balakishiyeva;D. Barker;
通讯作者：
R. Agnese;A. Anderson;T. Aralis;T. Aramaki;I. Arnquist;W. Baker;D. Balakishiyeva;D. Barker;
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
影响因子：
5
作者：
Akerib, D. S.;Alsum, S.;Zhang, C.
通讯作者：
Zhang, C.
用于暗物质搜索的超高纯度 NaI(Tl) 晶体的生长
影响因子：
4.2
作者：
Suerfu, Burkhant;Wada, Masayuki;Peloso, Winston;Souza, Michael;Calaprice, Frank;Tower, Joshua;Ciampi, Guido
通讯作者：
Ciampi, Guido