The Calibration of the Geometry and Antenna Delay in Askaryan Radio Array Station 4 and 5
The Calibration of the Geometry and Antenna Delay in Askaryan Radio Array Station 4 and 5
复制标题
阿斯卡扬无线电阵列站4和5的几何和天线延迟的校准
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发表时间：
2021
期刊：
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通讯作者：
J. Hanson
中科院分区：
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作者：
P. Dasgupta;K. Hughes;M. Beheler;P. Dasgupta;M. Huang;P. Allison;S. Archambault;J. Beatty;D. Besson;M. Beydler;C. Chen;P. Chen;Y. C. Chen;B. Clark;W. Clay;A. Connolly;L. Cremonesi;J. Davies;K. D. Vries;C. Deaconu;J. Flaherty;E. Friedman;R. Gaior;K. Hanson;N. Harty;B. Hendricks;K. Hoffman;B. Hokanson;E. Hong;S. Hsu;J. J. Huang;Melin Huang;K. Hughes;A. Ishihara;A. Karle;J. Kelley;R. Khandelwal;K. Kim;M.;R. Krebs;I. Kravchenko;Y. Ku;C. Kuo;K. Kurusu;U. Latif;A. Laundrie;H. Landsman;M. Lu;Tsung;B. Madison;K. Mase;T. Meures;J. Nam;A. Novikov;R. Nichol;G. Nir;A. Nozdrina;E. Oberla;A. O'Murchadha;J. Osborn;Y. Pan;C. Pfendner;N. Punsuebsay;J. Roth;P. Sandstrom;D. Seckel;Y. Shiao;A. Shultz;D. Smith;J. Torres;S. Toscano;J. Touart;N. Eijndhoven;G. Varner;A. Vieregg;M. Z. Wang;S. H. Wang;Y. Wang;S. Wissel;C. Xie;R. Young;S. Yoshida;M. B. Amass;S. D. Kockere;M. DuVernois;J. Hanson
位于南极的阿斯卡良射电阵列（ARA）实验旨在探测冰中超高能量宇宙中微子相互作用产生的射电信号。有5个独立的ARA站，其中一个（A5）包括一个低阈值相控阵触发串。每个ARA站都被设计成一个自主探测器。所有ARA站的数据采集系统都配备了冰射线采样器第二代（IRS2）芯片，这是一种定制的专用集成电路（ASIC），用于高速采样和数字化。在这篇文章中，我们描述了用于校准IRS2数字化芯片和观测站几何形状的方法，即部署在南极冰面以下200米的ARA 4站和5站的每对ARA天线之间的相对时间，以及它们在冰中的几何位置。我们的校准允许输入信号之间适当的时序相关性，这对于无线电顶点重建和通过阿斯卡扬效应检测超高能量中微子至关重要。我们实现了亚纳秒级的信号定时精度和10厘米以内的天线定位精度。
The Askaryan Radio Array (ARA) experiment at the South Pole is designed to detect the radio signals produced by ultra high energy cosmic neutrino interactions in the ice. There are 5 independent ARA stations, one of which (A5) includes a low-threshold phased array trigger string. Each ARA station is designed to work as an autonomous detector. The Data Acquisition System in all ARA stations is equipped with the Ice Ray Sampler second-generation (IRS2) chip, a custom-made, application-specific integrated circuit (ASIC) for high-speed sampling and digitization. In this contribution, we describe the methodology used to calibrate the IRS2 digitizer chip and the station geometry, namely the relative timing between each pair of ARA antennas, deployed at 200 m below the Antarctic ice surface, and their geometrical positions in the ice, for ARA stations 4 and 5. Our calibration allows for proper timing correlations between incoming signals, which is crucial for radio vertex reconstruction and thus detection of ultra high energy neutrinos through the Askaryan effect. We achieve a signal timing precision on a sub-nanosecond level and an antenna position precision within 10 cm.