Supernova neutrino detection in LZ
Supernova neutrino detection in LZ
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DOI：
10.1088/1748-0221/13/02/c02024
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发表时间：
2018-01
影响因子：
1.3
通讯作者：
D. Khaitan
中科院分区：
文献类型：
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作者：
D. Khaitan
在核心坍塌超新星的前10秒内，几乎所有其前身的引力势O(1053ergs)都以中微子的形式被带走。这些动能为O(10 MeV)的中微子可以通过相干弹性中微子-核散射(CEνNS)在探测器中沉积O(1keV)而相互作用。在这项工作中，我们描述了LUX-ZEPLIN(LZ)等低本底暗物质探测器在探测这些中微子相互作用方面的性能。例如，一颗27M⊙超新星在10kpc时预计将在LZ的7吨液体氙气活动体积中产生∼350中微子相互作用。基于LS220Eos中微子通量模型，采用诺布尔元素模拟技术(Nest)，并预测了CE-ν-NS截面，研究了SN中微子在LZ中的能量沉积和探测。我们模拟了LZ数据采集系统(DAQ)的响应，并展示了其处理这种交互速率的能力和局限性。我们介绍了LZ探测器的概况，重点介绍了液体氙气对超新星中微子探测的好处。我们讨论了能量沉积和探测器响应模拟及其结果。我们提出了一种分析技术来重建中微子总数和超新星核心反弹的时间。
In the first 10 seconds of a core-collapse supernova, almost all of its progenitor's gravitational potential, O(1053 ergs), is carried away in the form of neutrinos. These neutrinos, with O(10 MeV) kinetic energy, can interact via coherent elastic neutrino-nucleus scattering (CEνNS) depositing O(1 keV) in detectors. In this work we describe the performances of low-background dark matter detectors, such as LUX-ZEPLIN (LZ), optimized for detecting low-energy depositions, in detecting these neutrino interactions. For instance, a 27 M⊙ supernova at 10 kpc is expected to produce ∼350 neutrino interactions in the 7-tonne liquid xenon active volume of LZ. Based on the LS220 EoS neutrino flux model for a SN, the Noble Element Simulation Technique (NEST), and predicted CEνNS cross-sections for xenon, to study energy deposition and detection of SN neutrinos in LZ. We simulate the response of the LZ data acquisition system (DAQ) and demonstrate its capability and limitations in handling this interaction rate. We present an overview of the LZ detector, focusing on the benefits of liquid xenon for supernova neutrino detection. We discuss energy deposition and detector response simulations and their results. We present an analysis technique to reconstruct the total number of neutrinos and the time of the supernova core bounce.