Search for Point Sources of High-Energy Neutrinos with AMANDA
Search for Point Sources of High-Energy Neutrinos with AMANDA
复制标题
与 AMANDA 一起寻找高能中微子点源
DOI：
10.1086/345352
复制
发表时间：
2002
期刊：
影响因子：
--
通讯作者：
S. Young
中科院分区：
文献类型：
--
作者：
J. Ahrens;X. Bai;G. Barouch;S. Barwick;R. Bay;T. Becka;K. Becker;D. Bertrand;F. Binon;A. Biron;S. Boeser;O. Botner;A. Bouchta;O. Bouhali;T. Burgess;S. Carius;T. Castermans;D. Chirkin;J. Conrad;J. Cooley;D. Cowen;A. Davour;C. De Clercq;T. DeYoung;P. Desiati;J. Dewulf;P. Doksus;J. Edsjö;P. Ekström;T. Feser;T. Gaisser;M. Gaug;L. Gerhardt;A. Goldschmidt;A. Hallgren;F. Halzen;K. Hanson;R. Hardtke;T. Hauschildt;M. Hellwig;P. Herquet;G. Hill;P. O. Hulth;K. Hultqvist;S. Hundertmark;J. Jacobsen;A. Karle;J. Kim;L. Köpke;M. Kowalski;K. Kuehn;J. Lamoureux;H. Leich;M. Leuthold;P. Lindahl;J. Madsen;P. Marciniewski;H. Matis;C. Mcparland;T. Miller;Y. Minaeva;P. Miočinović;P. Mock;R. Morse;T. Neunhöffer;P. Niessen;D. Nygren;H. Ögelman;P. Olbrechts;C. Pérez de los Heros;A. Pohl;P. Price;G. Przybylski;K. Rawlins;E. Resconi;W. Rhode;M. Ribordy;S. Richter;J. Rodríguez Martino;P. Romenesko;D. Ross;H. Sander;T. Schmidt;D. Schneider;R. Schwarz;A. Silvestri;M. Solarz;G. Spiczak;C. Spiering;David Steele;P. Steffen;R. Stokstad;K. Sulanke;I. Taboada;L. Thollander;S. Tilav;C. Walck;C. Weinheimer;C. Wiebusch;C. Wiedemann;R. Wischnewski;H. Wissing;K. Woschnagg;W. Wu;G. Yodh;S. Young
本文描述了使用AMANDA-B10探测器寻找高能中微子的天文来源，AMANDA-B10探测器是一个由302个光电倍增管组成的阵列，用于探测深埋在南极冰中的上行中微子诱导的μ子产生的切伦科夫光。利用阿曼达探测器与地面上两台独立望远镜GASP空气切伦科夫望远镜和SPASE广延空气簇射阵列之间的重合事件，研究了绝对指向精度和角分辨率。利用1997年4月至10月（130.1天的生存时间）收集的数据，对北方半球进行了一次一般性调查，结果表明，从任何方向发生的事件在统计上都没有显著的增加。μ子中微子通量的灵敏度是基于对通过μ子的有效探测面积。在北方天空平均，对Eμ 10 TeV的有效探测面积超过10，000 m2。宇宙射线相互作用在大气中产生的中微子被用来验证探测器的预测性能。对于一个微分能谱与E成正比且斜率大于+40°的源，当能量阈值为10 GeV时，我们得到E ~ 2（dNν/dE）≤ 10 ~（-6）GeV cm ~（-2）s ~（-1）。
This paper describes the search for astronomical sources of high-energy neutrinos using the AMANDA-B10 detector, an array of 302 photomultiplier tubes used for the detection of Cerenkov light from upward-traveling neutrino-induced muons, buried deep in ice at the South Pole. The absolute pointing accuracy and angular resolution were studied by using coincident events between the AMANDA detector and two independent telescopes on the surface, the GASP air Cerenkov telescope and the SPASE extensive air shower array. Using data collected from 1997 April to October (130.1 days of live time), a general survey of the northern hemisphere revealed no statistically significant excess of events from any direction. The sensitivity for a flux of muon neutrinos is based on the effective detection area for through-going muons. Averaged over the northern sky, the effective detection area exceeds 10,000 m2 for Eμ ≈ 10 TeV. Neutrinos generated in the atmosphere by cosmic-ray interactions were used to verify the predicted performance of the detector. For a source with a differential energy spectrum proportional to E and declination larger than +40°, we obtain E2(dNν/dE) ≤ 10-6 GeV cm-2 s-1 for an energy threshold of 10 GeV.
DOI：
--
发表时间：
2000
期刊：
Astro Particle Physics 13
影响因子：
--
作者：
M.Teshima;他
通讯作者：
他
影响因子：
6.5
作者：
Hure;J.-M;Hersant;F.;Surville;C.;Nakai;N.;Jacq;T.
通讯作者：
T.