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The ZEPLIN III Galactic Dark Matter Search

ZEPLIN III 银河暗物质搜索

基本信息

批准号：
PP/E006841/1
负责人：
Timothy Sumner
金额：
$ 115.4万
依托单位：
Imperial College London
依托单位国家：
英国
项目类别：
Research Grant
财政年份：
2007
资助国家：
英国
起止时间：
2007 至无数据
项目状态：
已结题

来源：
https://gtr.ukri.org/projects?ref=PP%2FE006841%2F1
关键词：
ZEPLIN III Galactic Dark Matter

项目摘要

Please also see the PPARC publications and leaflets on dark matter. From the earliest times, observations have been made of the Universe. Since 1933 and the measurements of Fritz Zwicky, it has become apparent that the stars, planets, gas and everything else we know of in space, contributes only a few percent of the total mass of the Universe. The overwhelming evidence now suggests that about 1/3 of the remaining mass is in the form of so called dark matter, and about 2/3 is dark energy. What the dark matter and dark energy are has become one of the most important questions in science. The best candidate comes from particle physics. Here, our fundamental understanding of the basic building blocks of Nature suggests that all the particles we have ever seen, such as electrons, quarks and neutrinos, are in fact only half of all the particles that are 'out there'. In addition, there are 'supersymmetric' particles, and one of these, the lightest, is predicted to have precisely the properties needed to explain the dark matter. Hence, the prediction is that the stars we see wen we look up at the night sky are in fact only a small component of the Galaxy, the content in fact being dominated by a diffuse halo of very weakly interacting particles, known as WIMPs, through which the Sun and Earth are moving. It is the goal of the ZEPLIN-III collaboration to make the World's first direct detection of dark matter and these new particles. The ZEPLIN-III detector comprises an active target volume of 8 kg of xenon, kept cold enough to be a liquid. Occasionally, one of the WIMP particles of the dark matter through which the Earth is moving will scatter off an atom of the xenon, and when it does so it will generate a small flash of light and the liberation of a small amount of electrical charge. ZEPLIN-III is designed to be able to see these small signals, revealing the presence of the dark matter. The natural radiation of space (cosmic rays) could also do this, and so the detector has to be buried deep underground in a mine. The collaboration proposing the ZEPLIN-III project have great experience in this field. They have already completed the ZEPLIN-I project, are presently analysing data from the ZEPLIN-II detector, and have designed ZEPLIN-III to be the most sensitive dark matter experiment ever. The detector itself has already been built and tested, having been funded through previous PPARC grants. This grant application is to provide funds to allow deployment in the Boulby mine and exploitation over a period of 30 months. ZEPLIN-III is so sensitive that, in addition to going deep underground, an upgrade to lower radioactivity light detectors is required, as is the construction and implementation of a surrounding veto detector. Funds to cover these necessary aspects are also requested.

请参阅PPARC关于暗物质的出版物和传单。从最早的时候起，人们就对宇宙进行了观测。自从1933年弗里茨·兹威基的测量以来，很明显，恒星、行星、气体和我们所知道的太空中的一切，只占宇宙总质量的百分之几。现在压倒性的证据表明，剩余质量的大约1/3是所谓的暗物质，大约2/3是暗能量。暗物质和暗能量是什么已经成为科学中最重要的问题之一。最好的候选人来自粒子物理学。在这里，我们对自然界基本组成部分的基本理解表明，我们所见过的所有粒子，如电子，夸克和中微子，实际上只是“外面”所有粒子的一半。此外，还有“超对称”粒子，其中最轻的一种粒子被预测具有解释暗物质所需的精确性质。因此，我们在仰望夜空时看到的恒星实际上只是银河系的一小部分，其内容实际上是由一个非常弱相互作用的粒子（称为WIMP）组成的弥散光环所主导的，太阳和地球正在通过它移动。ZEPLIN-III合作的目标是实现世界上第一次直接探测暗物质和这些新粒子。ZEPLIN-III探测器包含一个8 kg氙的有效目标体积，保持足够冷以成为液体。偶尔，地球运动通过的暗物质的一个WIMP粒子会散射氙原子，当它这样做时，它会产生一个小闪光和少量电荷的释放。ZEPLIN-III被设计成能够看到这些小信号，揭示暗物质的存在。太空的自然辐射（宇宙射线）也可以做到这一点，因此探测器必须深埋在矿井的地下。提出ZEPLIN-III项目的合作伙伴在这一领域拥有丰富的经验。他们已经完成了ZEPLIN-I项目，目前正在分析来自ZEPLIN-II探测器的数据，并将ZEPLIN-III设计成有史以来最灵敏的暗物质实验。探测器本身已经建造和测试，由PPARC以前的赠款资助。该赠款申请将提供资金，以便在30个月内部署在Boulby矿和开采。ZEPLIN-III非常敏感，除了深入地下外，还需要升级到低放射性光探测器，以及建造和安装周围否决探测器。还需要资金来支付这些必要方面的费用。

项目成果

期刊论文数量（10）

专著数量（0）

科研奖励数量（0）

会议论文数量（0）

专利数量（0）

Detection of a single electron in xenon-based electroluminescent detectors

氙基电致发光探测器中单个电子的检测

DOI：
10.1134/s1063778809040103
发表时间：
2009
期刊：
Physics of Atomic Nuclei
影响因子：
0.4
作者：
Burenkov A
通讯作者：
Burenkov A

Measurements of neutrons produced by high-energy muons at the Boulby Underground Laboratory

鲍尔比地下实验室对高能 μ 子产生的中子的测量

DOI：
10.1016/j.astropartphys.2008.05.004
发表时间：
2008
期刊：
Astroparticle Physics
影响因子：
3.5
作者：
ARAUJO H
通讯作者：
ARAUJO H

WIMP-nucleon cross-section results from the second science run of ZEPLIN-III

DOI：
10.1016/j.physletb.2012.01.064
发表时间：
2011-10
期刊：
Physics Letters B
影响因子：
4.4
作者：
D. Akimov;H. Araújo;E. Barnes;V. Belov;A. Bewick;A. Burenkov;V. Chepel;A. Currie;L. deViveiros;B. Edwards;C. Ghag;A. Hollingsworth;M. Horn;W. Jones;G. Kalmus;A. Kobyakin;A. Kovalenko;V. Lebedenko;A. Lindote;A. Lindote;M. Lopes;R. Lüscher;P. Majewski;A. Murphy;F. Neves;F. Neves;S. Paling;J. G. D. Cunha;R. Preece;J. Quenby;L. Reichhart;P. Scovell;C. Silva;V. Solovov;N. Smith;V. Stekhanov;T. Sumner;C. Thorne;R. Walker
通讯作者：
D. Akimov;H. Araújo;E. Barnes;V. Belov;A. Bewick;A. Burenkov;V. Chepel;A. Currie;L. deViveiros;B. Edwards;C. Ghag;A. Hollingsworth;M. Horn;W. Jones;G. Kalmus;A. Kobyakin;A. Kovalenko;V. Lebedenko;A. Lindote;A. Lindote;M. Lopes;R. Lüscher;P. Majewski;A. Murphy;F. Neves;F. Neves;S. Paling;J. G. D. Cunha;R. Preece;J. Quenby;L. Reichhart;P. Scovell;C. Silva;V. Solovov;N. Smith;V. Stekhanov;T. Sumner;C. Thorne;R. Walker

Measurements and simulations of muon-induced neutrons

μ子感生中子的测量和模拟