Background studies for acoustic neutrino detection at the South Pole
Background studies for acoustic neutrino detection at the South Pole
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南极声中微子探测的背景研究
DOI：
10.1016/j.astropartphys.2011.09.004
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发表时间：
2011
影响因子：
3.5
通讯作者：
P. Zarzhitsky
中科院分区：
文献类型：
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作者：
T. I. C. R. Abbasi;Y. Abdou;T. Abu;J. Adams;J. Aguilar;M. Ahlers;K. Andeen;J. Auffenberg;X. Bai;M. Baker;S. Barwick;R. Bay;J. Alba;K. Beattie;J. Beatty;S. Bechet;J. Becker;K. Becker;M. Benabderrahmane;S. BenZvi;J. Berdermann;P. Berghaus;D. Berley;E. Bernardini;D. Bertrand;D. Besson;D. Bindig;M. Bissok;E. Blaufuss;J. Blumenthal;D. Boersma;C. Bohm;D. Bose;S. Boser;O. Botner;J. Braun;A. Brown;S. Buitink;M. Carson;D. Chirkin;B. Christy;J. Clem;F. Clevermann;S. Cohen;C. Colnard;D. Cowen;M. D'Agostino;M. Danninger;J. Daughhetee;J. Davis;C. Clercq;L. Demirors;T. Denger;O. Depaepe;F. Descamps;P. Desiati;G. Vries;T. DeYoung;J. C. Diaz;M. Dierckxsens;J. Dreyer;J. Dumm;R. Ehrlich;J. Eisch;R. Ellsworth;O. Engdegaard;S. Euler;P. Evenson;O. Fadiran;A. Fazely;A. Fedynitch;T. Feusels;K. Filimonov;C. Finley;T. Fischer;M. Foerster;B. Fox;A. Franckowiak;R. Franke;T. Gaisser;J. Gallagher;M. Geisler;L. Gerhardt;L. Gladstone;T. Glusenkamp;A. Goldschmidt;J. Goodman;D. Grant;T. Griesel;A. Gross;S. Grullon;M. Gurtner;C. Ha;A. Hallgren;F. Halzen;K. Han;K. Hanson;D. Heinen;K. Helbing;P. Herquet;S. Hickford;G. Hill;K. Hoffman;A. Homeier;K. Hoshina;Daan Hubert;W. Huelsnitz;J. Hulss;P. O. Hulth;K. Hultqvist;S. Hussain;A. Ishihara;J. Jacobsen;G. Japaridze;H. Johansson;J. Joseph;K. Kampert;A. Kappes;T. Karg;A. Karle;J. Kelley;P. Kenny;J. Kiryluk;F. Kislat;S. Klein;J. Kohne;G. Kohnen;H. Kolanoski;L. Kopke;S. Kopper;D. Koskinen;M. Kowalski;T. Kowarik;M. Krasberg;T. Krings;G. Kroll;K. Kuehn;T. Kuwabara;M. Labare;S. Lafebre;K. Laihem;H. Landsman;M. Larson;R. Lauer;J. Lunemann;J. Madsen;P. Majumdar;A. Marotta;R. Maruyama;K. Mase;H. Matis;K. Meagher;M. Merck;P. M'esz'aros;T. Meures;E. Middell;N. Milke;J. Miller;T. Montaruli;R. Morse;S. Movit;R. Nahnhauer;J. Nam;U. Naumann;P. Niessen;D. Nygren;S. Odrowski;A. Olivas;M. Olivo;A. O'Murchadha;M. Ono;S. Panknin;L. Paul;C. Heros;J. Petrovic;A. Piegsa;D. Pieloth;R. Porrata;J. Posselt;P. Price;M. Prikockis;G. Przybylski;K. Rawlins;P. Redl;E. Resconi;W. Rhode;M. Ribordy;A. Rizzo;J. Rodrigues;P. Roth;F. Rothmaier;C. Rott;T. Ruhe;D. Rutledge;B. Ruzybayev;D. Ryckbosch;H. Sander;M. Santander;S. Sarkar;K. Schatto;T. Schmidt;A. Schonwald;A. Schukraft;A. Schultes;O. Schulz;M. Schunck;D. Seckel;B. Semburg;S. Seo;Y. Sestayo;S. Seunarine;A. Silvestri;A. Slipak;G. Spiczak;C. Spiering;M. Stamatikos;T. Stanev;G. Stephens;T. Stezelberger;R. Stokstad;A. Stossl;S. Stoyanov;E. Strahler;T. Straszheim;M. Stur;G. Sullivan;Q. Swillens;H. Taavola;I. Taboada;A. Tamburro;A. Tepe;S. Ter;S. Tilav;P. Toale;S. Toscano;D. Tosi;D. Turvcan;N. Eijndhoven;J. Vandenbroucke;A. Overloop;J. Santen;M. Vehring;M. Voge;C. Walck;T. Waldenmaier;M. Wallraff;M. Walter;C. Weaver;C. Wendt;S. Westerhoff;N. Whitehorn;K. Wiebe;C. Wiebusch;D. Williams;R. Wischnewski;H. Wissing;M. Wolf;K. Woschnagg;C. Xu;X. Xu;J. Yáñez;G. Yodh;S. Yoshida;P. Zarzhitsky
超高能中微子相互作用声信号的探测是一种很有前途的测量地球上宇宙成因中微子微小通量的方法。该过程的能量阈值强烈依赖于靶材料中的绝对噪声水平。南极声学测试装置（SPATS）部署在IceCube中微子观测站四个钻孔的上部，两年多来一直监测南极冰中500米深处的噪音。噪声是非常稳定和高斯分布。到目前为止，由于缺乏现场校准，一直使用实验室测量来估计10至50 kHz频率范围内的绝对噪声水平小于20 mPa。使用阈值触发器，南极声学测试装置的传感器记录了冰立方探测器体积及其附近的声脉冲状事件。来自再冻结冰立方洞和人为源的声信号已被用来定位声事件。从建立的源到SPATS传感器的声音传播的蒙特卡罗模拟允许检查相应的模型预期。能量为GeV的中微子通量的上限来自于八个月的声学数据。
The detection of acoustic signals from ultra-high energy neutrino interactions is a promising method to measure the tiny flux of cosmogenic neutrinos expected on Earth. The energy threshold for this process depends strongly on the absolute noise level in the target material. The South Pole Acoustic Test Setup (SPATS), deployed in the upper part of four boreholes of the IceCube Neutrino Observatory, has monitored the noise in Antarctic ice at the geographic South Pole for more than two years down to 500 m depth. The noise is very stable and Gaussian distributed. Lacking an in-situ calibration up to now, laboratory measurements have been used to estimate the absolute noise level in the 10 to 50 kHz frequency range to be smaller than 20 mPa. Using a threshold trigger, sensors of the South Pole Acoustic Test Setup registered acoustic pulse-like events in the IceCube detector volume and its vicinity. Acoustic signals from refreezing IceCube holes and from anthropogenic sources have been used to localize acoustic events. Monte Carlo simulations of sound propagating from the established sources to the SPATS sensors have allowed to check corresponding model expectations. An upper limit on the neutrino flux at energiesGeV is derived from acoustic data taken over eight months.
IceCube中微子望远镜第一年的性能，天体粒子物理学
DOI：
--
发表时间：
2006
期刊：
Astroparticle Physics 26
影响因子：
--
作者：
A.Achterberg et al.
通讯作者：
A.Achterberg et al.