Design, Construction and Operation of a Low-Power, Autonomous Radio-Frequency Data-Acquisition Station for the TARA Experiment
S. Kunwar, R. Abbasi, C. Allen, J. Belz, D. Besson, M. Byrne, B. Farhang-Boroujeny, W. H. Gillman, W. Hanlon, J. Hanson, I. Myers, A. Novikov, S. Prohira, K. Ra… 展开作者
S. Kunwar, R. Abbasi, C. Allen, J. Belz, D. Besson, M. Byrne, B. Farhang-Boroujeny, W. H. Gillman, W. Hanlon, J. Hanson, I. Myers, A. Novikov, S. Prohira, K. Ratzlaff, A. Rezazadeh, V. Sanivarapu, D. Schurig, A. Shustov, M. Smirnova, H. Takai, G. B. Thomson, R. Young
备注：
version accepted for publication in Nucl. Instr. Meth. A
Employing a 40-kW radio-frequency transmitter just west of Delta, UT, and operating at 54.1 MHz, the TARA (Telescope Array RAdar) experiment seeks radar detection of extensive air showers (EAS) initiated by ultra-high energy cosmic rays (UHECR). For UHECR with energies in excess of $10^{19}$ eV, the Doppler-shifted "chirps" resulting from EAS shower core radar reflections should be observable above background (dominantly galactic) at distances of tens of km from the TARA transmitter. In order to stereoscopically reconstruct cosmic ray chirps, two remote, autonomous self-powered receiver stations have been deployed. Each remote station (RS) combines both low power consumption as well as low cost. Triggering logic, the powering and communication systems, and some specific details of hardware components are discussed.
Pulsar Backend for 21 CentiMeter Array: Implementation of Data Acquisition and Initial Results
Peking University（北京大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；State Key Laboratory of Radio Astronomy and Technology, National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台射电天文与技术重点实验室）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Xinjiang Astronomical Observatory, Chinese Academy of Sciences（中国科学院新疆天文台）
The Array Control and Data Acquisition software of the Cherenkov Telescope Array Observatory
CIEMAT（西班牙核能研究中心）；CTAO ERIC, Science Data Management Centre (SDMC)（切伦科夫望远镜阵列观测站欧洲研究基础设施联盟科学数据管理中心）；Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physiquedes Particules-IN2P3（萨瓦-上萨瓦大学）；Département d’Astronomie, Université de Genève（日内瓦大学）；Institut d’Estudis Espacials de Catalunya(IEEC)（加泰罗尼亚空间研究所）；Deutsches Elektronen-Synchrotron DESY（德国电子同步辐射中心）；INAF, Osservatorio Astrofisico di Catania（意大利国家天体物理研究所卡塔尼亚天文台）；COSYLAB JSC, Control System Laboratory（COSYLAB股份公司）；INAF/OAS Bologna（意大利国家天体物理研究所博洛尼亚天文台）；CNRS/IN2P3, CPPM, Aix Marseille Univ（艾克斯-马赛大学）
Some possible interpretations from data of the CODALEMA experiment
安装在南赛射电天文台（法国）的CODALEMA实验的目的是研究$10^{16}-10^{18} eV$能量范围内的超高能宇宙射线的无线电探测。分布在0.25 km $^2$的区域内，原始设备同时使用粒子探测器阵列和短天线阵列，并进行集中采集。在考虑地磁场影响的情况下，给出了无线电能量观测量的新分析。自2011年以来，在初始配置周围1.5公里$^2$的区域内部署了由60个独立和自触发台站组成的新的无线电探测器阵列。这一新的发展导致了具体的限制，要讨论的方面，宇宙射线的识别和分析的波前。
