Lunar detection of ultra-high-energy cosmic rays and neutrinos with the Square Kilometre Array
J. D. Bray, J. Alvarez-Muñiz, S. Buitink, R. D. Dagkesamanskii, R. D. Ekers, H. Falcke, K. G. Gayley, T. Huege, C. W. James, M. Mevius, R. L. Mutel, R. J. Proth… 展开作者
J. D. Bray, J. Alvarez-Muñiz, S. Buitink, R. D. Dagkesamanskii, R. D. Ekers, H. Falcke, K. G. Gayley, T. Huege, C. W. James, M. Mevius, R. L. Mutel, R. J. Protheroe, O. Scholten, R. E. Spencer, S. ter Veen
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Contribution to the conference on "Advancing Astrophysics with the Square Kilometre Array" for the SKA science book; revised, accepted version
The origin of the most energetic particles in nature, the ultra-high-energy (UHE) cosmic rays, is still a mystery. Only the most energetic of these have sufficiently small angular deflections to be used for directional studies, and their flux is so low that even the 3,000 km^2 Pierre Auger detector registers only about 30 cosmic rays per year of these energies. A method to provide an even larger aperture is to use the lunar Askaryan technique, in which ground-based radio telescopes search for the nanosecond radio flashes produced when a cosmic ray interacts with the Moon's surface. The technique is also sensitive to UHE neutrinos, which may be produced in the decays of topological defects from the early universe.
Observations with existing radio telescopes have shown that this technique is technically feasible, and established the required procedure: the radio signal should be searched for pulses in real time, compensating for ionospheric dispersion and filtering out local radio interference, and candidate events stored for later analysis. For the Square Kilometre Array (SKA), this requires the formation of multiple tied-array beams, with high time resolution, covering the Moon, with either SKA1-LOW or SKA1-MID. With its large collecting area and broad bandwidth, the SKA will be able to detect the known flux of UHE cosmic rays using the visible lunar surface - millions of square km - as the detector, providing sufficient detections of these extremely rare particles to address the mystery of their origin.
Comprehensive Study of the Lunar Energetic Particle Environment with LunPAN
University of Geneva（日内瓦大学）；Czech Technical University in Prague（布拉格捷克理工大学）；University of West Bohemia（西波希米亚大学）；Aerospacelab S.A.（航空航天实验室股份有限公司）；European Organization for Nuclear Research (CERN)（欧洲核子研究组织（欧洲核子研究中心））
Design and performance of the coded mask for the Lunar Electromagnetic Monitor in X-rays (LEM-X)
INAF, Istituto di Astrofisica e Planetologia Spaziali（意大利国家天体物理研究所，空间天体物理学与行星学研究所）；INFN, Sez. Roma Tor Vergata（意大利国家核物理研究所，罗马托维加塔分部）；University of Rome “La Sapienza”, Dept. of Physics（罗马大学，物理系）；INAF, Osservatorio Astronomico di Roma（意大利国家天体物理研究所，罗马天文台）；Agenzia Spaziale Italiana（意大利航天局）；INAF, Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所，天体物理学与空间科学观测站）；INFN, Sez. Bologna（意大利国家核物理研究所，博洛尼亚分部）
Physical Insights, LLC.（物理洞察有限公司）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Purdue University（普渡大学）；Hawaii Institute of Geophysics and Planetology（夏威夷地球物理与行星研究所）；University of Chicago（芝加哥大学）
Galactic Cosmic Rays and Solar Energetic Particles in Cis-Lunar Space: Need for contextual energetic particle measurements at Earth and supporting distributed observations
CHEC: A Compact High Energy Camera for the Cherenkov Telescope Array
切伦科夫望远镜阵列将提供前所未有的灵敏度和角分辨率的伽马射线跨越数量级的能量。在1 TeV以上到300 TeV左右，小型望远镜阵列（SST）将覆盖地面上的几公里。紧凑型高能相机（CHEC）是SST相机的建议选项。CHEC包含2048个像素，物理尺寸约为6 mm x 6 mm，导致超过8度的视场。基于定制ASIC（TARGET）和FPGA的电子器件以每秒千兆采样的速度对输入信号进行采样，并提供灵活的触发方案。每个事件中每个像素的波形以每秒超过600个事件的速度无损失地读出。位于巴黎默东的望远镜原型在2015年底使用第一个CHEC原型从空气淋浴中看到了第一个切伦科夫光。CHEC的研究和开发目前集中在利用最新一代的硅光电倍增器（SiPM）。
A Search for Effects of Cosmic Rays with Multi-scale Entropy Metrics
National Quantum Computing Testbed, School of Mathematics and Physics, University of Queensland（昆士兰大学数学与物理学院国家量子计算测试床）；Quantum Technologies and Dark Matter Labs, Department of Physics, University of Western Australia（西澳大利亚大学物理系量子技术与暗物质实验室）；Centre for Astrophysics and Supercomputing, Swinburne University of Technology（斯威本科技大学天体物理学与超级计算中心）；Wenzel Associates Inc.（温泽尔合伙公司）
