费尔森凯勒浅层地下实验室的一个新的超低水平HPGe活动计数装置

IF 4.2 3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS
S. Turkat , D. Bemmerer , A. Boeltzig , A.R. Domula , J. Koch , T. Lossin , M. Osswald , K. Schmidt , K. Zuber
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引用次数: 1

摘要

德国德累斯顿费尔森凯勒浅层地下实验室安装了一种新的超低能级计数装置。它包括一个高纯度锗探测器(HPGe),在被动和主动屏蔽内的相对效率为163%。被动屏蔽层由45米的岩石覆盖层(相当于140米的水),40厘米的低活性混凝土和一个由防氡盒包围的铅和铜城堡组成。研究发现,单是被动屏蔽就能将本底辐射率降低到与其他浅层地下实验室相当的水平。另外一个积极的否决是由周围设置的五个大型塑料闪烁板给出的。在[40 keV;2700 keV]的能量区间内,它进一步将背景速率降低了一个数量级以上,降至116(1)kg−1d−1。如此低的本底率对于浅层地下实验室和接近深层地下实验室来说是前所未有的。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
A new ultra low-level HPGe activity counting setup in the Felsenkeller shallow-underground laboratory

A new ultra low-level counting setup has been installed in the shallow-underground laboratory Felsenkeller in Dresden, Germany. It includes a high-purity germanium detector (HPGe) of 163% relative efficiency within passive and active shields. The passive shield consists of 45 m rock overburden (140 meters water equivalent), 40 cm of low-activity concrete, and a lead and copper castle enclosed by an anti-radon box. The passive shielding alone is found to reduce the background rate to rates comparable to other shallow-underground laboratories. An additional active veto is given by five large plastic scintillation panels surrounding the setup. It further reduces the background rate by more than one order of magnitude down to 116(1) kg−1d−1 in an energy interval of [40 keV;2700 keV]. This low background rate is unprecedented for shallow-underground laboratories and close to deep underground laboratories.

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来源期刊
Astroparticle Physics
Astroparticle Physics 地学天文-天文与天体物理
CiteScore
8.00
自引率
2.90%
发文量
41
审稿时长
79 days
期刊介绍: Astroparticle Physics publishes experimental and theoretical research papers in the interacting fields of Cosmic Ray Physics, Astronomy and Astrophysics, Cosmology and Particle Physics focusing on new developments in the following areas: High-energy cosmic-ray physics and astrophysics; Particle cosmology; Particle astrophysics; Related astrophysics: supernova, AGN, cosmic abundances, dark matter etc.; Gravitational waves; High-energy, VHE and UHE gamma-ray astronomy; High- and low-energy neutrino astronomy; Instrumentation and detector developments related to the above-mentioned fields.
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