SEARCHES FOR HIGH-ENERGY NEUTRINO EMISSION IN THE GALAXY WITH THE COMBINED ICECUBE

DOI：

10.1088/0004-637x/763/1/33

发表时间：

2012-10

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

I. R. Abbasi;Y. Abdou;M. Ackermann;J. Adams;J. Aguilar;M. Ahlers;D. Altmann;K. Andeen;J. Auffenberg;X. Bai;M. Baker;S. Barwick;V. Baum;R. Bay;K. Beattie;J. Beatty;S. Bechet;J. Tjus;K. Becker;M. Bell;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;L. Brayeur;A. Brown;R. Bruijn;J. Brunner;S. Buitink;M. Carson;J. Casey;M. Casier;D. Chirkin;B. Christy;F. Clevermann;S. Cohen;D. Cowen;A. H. C. Silva;M. Danninger;J. Daughhetee;J. Davis;C. Clercq;F. Descamps;P. Desiati;G. D. V. Uiterweerd;T. DeYoung;J. C. D'iaz-V'elez;J. Dreyer;J. Dumm;M. Dunkman;R. Eagan;J. Eisch;R. Ellsworth;O. Engdegaard;S. Euler;P. Evenson;O. Fadiran;A. Fazely;A. Fedynitch;J. Feintzeig;T. Feusels;K. Filimonov;C. Finley;T. Fischer-Wasels;S. Flis;A. Franckowiak;R. Franke;K. Frantzen;T. Fuchs;T. Gaisser;J. Gallagher;L. Gerhardt;L. Gladstone;T. Glusenkamp;A. Goldschmidt;J. Goodman;D. G'ora;D. Grant;A. Gross;S. Grullon;M. Gurtner;C. Ha;A. H. Ismail;A. Hallgren;F. Halzen;K. Hanson;D. Heereman;P. Heimann;D. Heinen;K. Helbing;R. Hellauer;S. Hickford;G. Hill;K. Hoffman;R. Hoffmann;A. Homeier;K. Hoshina;W. Huelsnitz;P. O. Hulth;K. Hultqvist;S. Hussain;A. Ishihara;E. Jacobi;J. Jacobsen;G. Japaridze;O. Jlelati;A. Kappes;T. Karg;A. Karle;J. Kiryluk;F. Kislat;J. Klas;S. Klein;J. Kohne;G. Kohnen;H. Kolanoski;L. Kopke;C. Kopper;S. Kopper;D. Koskinen;M. Kowalski;M. Krasberg;G. Kroll;J. Kunnen;N. Kurahashi;T. Kuwabara;M. Labare;K. Laihem;H. Landsman;M. Larson;R. Lauer;M. Lesiak-Bzdak;J. Lunemann;J. Madsen;R. Maruyama;K. Mase;H. Matis;F. McNally;K. Meagher;M. Merck;P. M'esz'aros;T. Meures;S. Miarecki;E. Middell;N. Milke;J. Miller;L. Mohrmann;T. Montaruli;R. Morse;S. Movit;R. Nahnhauer;U. Naumann;S. Nowicki;D. Nygren;A. Obertacke;S. Odrowski;A. Olivas;M. Olivo;A. O'Murchadha;S. Panknin;L. Paul;J. Pepper;C. Heros;D. Pieloth;N. Pirk;J. Posselt;P. Price;G. Przybylski;L. Radel;K. Rawlins;P. Redl;E. Resconi;W. Rhode;M. Ribordy;M. Richman;B. Riedel;J. Rodrigues;F. Rothmaier;C. Rott;T. Ruhe;B. Ruzybayev;D. Ryckbosch;S. M. Saba;T. Salameh;H. Sander;M. Santander;S. Sarkar;K. Schatto;M. Scheel;F. Scheriau;T. Schmidt;M. Schmitz;S. Schoenen;S. Schoneberg;L. Schonherr;A. Schonwald;A. Schukraft;L. Schulte;O. Schulz;D. Seckel;S. Seo;Y. Sestayo;S. Seunarine;M. Smith;M. Soiron;D. Soldin;G. Spiczak;C. Spiering;M. Stamatikos;T. Stanev;Alexander Stasik;T. Stezelberger;R. Stokstad;A. Stossl;E. Strahler;R. Strom;G. Sullivan;H. Taavola;I. Taboada;A. Tamburro;S. Ter-Antonyan;S. Tilav;P. Toale;S. Toscano;M. Usner;D. V. D. Drift-D.-V.-D.-Drift-103030812;N. Eijndhoven;A. Overloop;J. Santen;M. Vehring;M. Voge;C. Walck;T. Waldenmaier;M. Wallraff;M. Walter;R. Wasserman;C. Weaver;C. Wendt;S. Westerhoff;N. Whitehorn;K. Wiebe;C. Wiebusch;D. Williams;H. Wissing;M. Wolf;T. R. Wood;K. Woschnagg;C. Xu;D. Xu;X. Xu;J. Yáñez;G. Yodh;S. Yoshida;P. Zarzhitsky;J. Ziemann;A. Zilles;M. Zoll

我们报告了利用南极中微子望远镜、IceCube 和 AMANDA 收集的数据，在银河平面北部天空寻找能量高于 200 GeV 的中微子源。这项工作中考虑的银河区域包括朝向天鹅座区域的本地旋臂以及距离我们最近的英仙座旋臂。搜索基于 2007 年至 2009 年期间收集的数据。在此期间，AMANDA 是 IceCube 的一个组成部分，该冰立方仍在建设中，并通过部署在冰中的 22 串（2007-2008 年）和 40 串（2008-2009 年）光学模块进行运行。通过将更大的 IceCube 探测器的优点与更紧凑的 AMANDA 探测器的较低能量阈值相结合，我们在能量低于 ∼10 TeV 时相对于之前的搜索获得了更高的灵敏度。这里介绍的分析是对银河平面内点源的扫描，对天鹅座区域中多个和扩展源的优化搜索，这可能低于点源扫描的灵敏度，以及对七个预选中微子源候选的研究。其中之一“天鹅座 X-3”已经在观测到的射电和 X 射线耀斑的同时进行了中微子发射的时间依赖性搜索。没有发现信号证据，并且报告每次搜索的上限。我们研究与 E−2 和 E−3 成比例的中微子光谱，以覆盖可能的中微子光谱的整个范围。急剧下降的 E−3 中微子能谱也可用于近似能量截止值低于 50 TeV 的中微子能谱，因为这会导致探测器中事件的类似能量分布。对于北方天空可见的银道面区域，对于能量区域[180.0 GeV–20.5 TeV]的点状中微子源，90%置信度μ子中微子通量上限在E3dN/dE ∼ 5.4–19.5 × 10−11 TeV2 cm−2 s−1 范围内。这些代表了迄今为止报道的银河系内软谱中微子源最严格的上限。

We report on searches for neutrino sources at energies above 200 GeV in the Northern sky of the Galactic plane, using the data collected by the South Pole neutrino telescope, IceCube, and AMANDA. The Galactic region considered in this work includes the local arm toward the Cygnus region and our closest approach to the Perseus Arm. The searches are based on the data collected between 2007 and 2009. During this time AMANDA was an integrated part of IceCube, which was still under construction and operated with 22 strings (2007–2008) and 40 strings (2008–2009) of optical modules deployed in the ice. By combining the advantages of the larger IceCube detector with the lower energy threshold of the more compact AMANDA detector, we obtain an improved sensitivity at energies below ∼10 TeV with respect to previous searches. The analyses presented here are a scan for point sources within the Galactic plane, a search optimized for multiple and extended sources in the Cygnus region, which might be below the sensitivity of the point source scan, and studies of seven pre-selected neutrino source candidates. For one of them, Cygnus X-3, a time-dependent search for neutrino emission in coincidence with observed radio and X-ray flares has been performed. No evidence of a signal is found, and upper limits are reported for each of the searches. We investigate neutrino spectra proportional to E−2 and E−3 in order to cover the entire range of possible neutrino spectra. The steeply falling E−3 neutrino spectrum can also be used to approximate neutrino energy spectra with energy cutoffs below 50 TeV since these result in a similar energy distribution of events in the detector. For the region of the Galactic plane visible in the Northern sky, the 90% confidence level muon neutrino flux upper limits are in the range E3dN/dE ∼ 5.4–19.5 × 10−11 TeV2 cm−2 s−1 for point-like neutrino sources in the energy region [180.0 GeV–20.5 TeV]. These represent the most stringent upper limits for soft-spectra neutrino sources within the Galaxy reported to date.

SEARCHES FOR HIGH-ENERGY NEUTRINO EMISSION IN THE GALAXY WITH THE COMBINED ICECUBE–AMANDA DETECTOR

文献摘要

相似文献