Probing the angular and polarization reconstruction of the ARIANNA detector at the South Pole
Probing the angular and polarization reconstruction of the ARIANNA detector at the South Pole
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探索南极 ARIANNA 探测器的角度和偏振重建
DOI：
10.1088/1748-0221/15/09/p09039
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发表时间：
2020
影响因子：
1.3
通讯作者：
C. Glaser)
中科院分区：
文献类型：
--
作者：
ARIANNA collaboration (…;C. Glaser)
超高能（UHE）宇宙射线的来源，它可以有能量高达10 - 20 eV，仍然是一个谜。UHE中微子可能为理解宇宙射线源的性质提供重要线索。ARIANNA的目标是通过无线电（Askaryan）从粒子簇射发射中微子时，中微子与冰相互作用，这是一个有效的方法，中微子的能量在10 - 16 eV和10 - 20 eV。阿丽亚娜无线电探测器位于南极冰层表面之下。中微子观测要求无线电脉冲以最小的冰和雪介质失真传播到地面的天线。利用南极冰芯项目的剩余洞，从雪面以下1.7公里处的发射机发射了无线电脉冲。通过测量这些信号与ARIANNA地面站，角度和偏振重建能力进行了量化，这是需要测量的中微子的方向。在对探测器响应的原始信号和通过冰传播的衰减进行去卷积之后，信号脉冲没有显示出明显的失真，并且与在消声室中进行的发射器的参考测量一致。此外，信号脉冲揭示没有显着的双折射，我们测试的几何形状，主要是垂直冰传播。对发射的无线电脉冲的起源进行了测量，角分辨率为0.37 °，表明如果能很好地确定无线电脉冲的偏振，就能很好地确定中微子的方向。在本研究中，我们得到了2.7 o的偏振矢量的分辨率。这两项衡量都没有显示出与预期的重大偏差。
The sources of ultra-high energy (UHE) cosmic rays, which can have energies up to 10 20 eV, remain a mystery. UHE neutrinos may provide important clues to understanding the nature of cosmic-ray sources. ARIANNA aims to detect UHE neutrinos via radio (Askaryan) emission from particle showers when a neutrino interacts with ice, which is an efficient method for neutrinos with energies between 10 16 eV and 10 20 eV. The ARIANNA radio detectors are located in Antarctic ice just beneath the surface. Neutrino observation requires that radio pulses propagate to the antennas at the surface with minimum distortion by the ice and firn medium. Using the residual hole from the South Pole Ice Core Project, radio pulses were emitted from a transmitter located up to 1.7 km below the snow surface. By measuring these signals with an ARIANNA surface station, the angular and polarization reconstruction abilities are quantified, which are required to measure the direction of the neutrino. After deconvolving the raw signals for the detector response and attenuation from propagation through the ice, the signal pulses show no significant distortion and agree with a reference measurement of the emitter made in an anechoic chamber. Furthermore, the signal pulses reveal no significant birefringence for our tested geometry of mostly vertical ice propagation. The origin of the transmitted radio pulse was measured with an angular resolution of 0.37 o indicating that the neutrino direction can be determined with good precision if the polarization of the radio-pulse can be well determined. In the present study we obtained a resolution of the polarization vector of 2.7 o. Neither measurement show a significant offset relative to expectation.
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利用 ARIANNA 记录的无线电信号研究冰和发射器特性
DOI：
10.22323/1.358.0939
发表时间：
2019
期刊：
Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019)
影响因子：
--
作者：
R. Lahmann
通讯作者：
R. Lahmann
通过 ARIANNA 实验瞄准超高能中微子
影响因子：
2.6
作者：
ARIANNA collaboration (…;C. Glaser)
通讯作者：
C. Glaser)
影响因子：
6.4
作者：
Allison, P.;Archambault, S.;Beatty, J.J.;Besson, D.Z.;Chen, C.C.;Chen, C.H.;Chen, P.;Christenson, A.;Clark, B.A.;Clay, W.
通讯作者：
Clay, W.
使用 RICE 探测器对南极冰原进行原位折射率测量
影响因子：
3.4
作者：
I. Kravchenko;D. Besson;J. Meyers
通讯作者：
J. Meyers
DOI：
10.1140/epjc/s10052-020-7612-8
发表时间：
2019-06
期刊：
The European Physical Journal C
影响因子：
--
作者：
C. Glaser;Daniel Garc'ia-Fern'andez;A. Nelles;J. Alvarez-Muñiz;S. Barwick;D. Besson;B. Clark;A. Connolly;C. Deaconu;Krijn de Vries;J. Hanson;B. Hokanson-Fasig;R. Lahmann;U. Latif;S. Kleinfelder;C. Persichilli;Yue Pan;Carl Pfender;I. Plaisier;D. Seckel;J. Torres;S. Toscano;N. Eijndhoven;A. Vieregg;C. Welling;T. Winchen;S. Wissel
通讯作者：
C. Glaser;Daniel Garc'ia-Fern'andez;A. Nelles;J. Alvarez-Muñiz;S. Barwick;D. Besson;B. Clark;A. Connolly;C. Deaconu;Krijn de Vries;J. Hanson;B. Hokanson-Fasig;R. Lahmann;U. Latif;S. Kleinfelder;C. Persichilli;Yue Pan;Carl Pfender;I. Plaisier;D. Seckel;J. Torres;S. Toscano;N. Eijndhoven;A. Vieregg;C. Welling;T. Winchen;S. Wissel