Search for steady point-like sources in the astrophysical muon neutrino flux with 8 years of IceCube data
Search for steady point-like sources in the astrophysical muon neutrino flux with 8 years of IceCube data
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DOI：
10.1140/epjc/s10052-019-6680-0
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发表时间：
2018-11
期刊：
影响因子：
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通讯作者：
M. Aartsen;M. Ackermann;J. Adams;J. Aguilar;M. Ahlers;M. Ahrens;D. Altmann;K. Andeen;T. Anderson;I. Ansseau;G. Anton;C. Argüelles;J. Auffenberg;S. Axani;P. Backes;H. Bagherpour;X. Bai;A. Barbano;J. P. Barron;S. Barwick;V. Baum;R. Bay;J. Beatty;J. Becker Tjus;K. Becker;S. BenZvi;D. Berley;E. Bernardini;D. Besson;G. Binder;D. Bindig;E. Blaufuss;S. Blot;C. Bohm;M. Börner;F. Bos;S. Böser;O. Botner;E. Bourbeau;J. Bourbeau;F. Bradascio;J. Braun;H. Bretz;S. Bron;J. Brostean-Kaiser;A. Burgman;R. Busse;T. Carver;C. Chen;E. Cheung;D. Chirkin;K. Clark;L. Classen;G. Collin;J. Conrad;P. Coppin;P. Correa;D. Cowen;R. Cross;P. Dave;M. Day;J. D. André;C. Clercq;J. DeLaunay;H. Dembinski;K. Deoskar;S. Ridder;P. Desiati;K. D. Vries;G. Wasseige;M. With;T. DeYoung;J. C. Díaz-Vélez;H. Dujmovic;M. Dunkman;E. Dvorak;B. Eberhardt;T. Ehrhardt;B. Eichmann;P. Eller;P. Evenson;S. Fahey;A. Fazely;J. Felde;K. Filimonov;C. Finley;A. Franckowiak;E. Friedman;A. Fritz;T. Gaisser;J. Gallagher;E. Ganster;S. Garrappa;L. Gerhardt;K. Ghorbani;W. Giang;T. Glauch;T. Glüsenkamp;A. Goldschmidt;J. G. Gonzalez;D. Grant;Z. Griffith;C. Haack;A. Hallgren;L. Halve;F. Halzen;K. Hanson;D. Hebecker;D. Heereman;K. Helbing;R. Hellauer;S. Hickford;J. Hignight;G. Hill;K. Hoffman;R. Hoffmann;T. Hoinka;B. Hokanson-Fasig;K. Hoshina;F. Huang;M. Huber;K. Hultqvist;Mirco Hünnefeld;R. Hussain;S. In;N. Iovine;A. Ishihara;E. Jacobi;G. Japaridze;M. Jeong;K. Jero;B. Jones;P. Kalaczyński;W. Kang;A. Kappes;D. Kappesser;T. Karg;A. Karle;U. Katz;M. Kauer;A. Keivani;J. Kelley;A. Kheirandish;J. Kim;T. Kintscher;J. Kiryluk;T. Kittler;S. Klein;R. Koirala;H. Kolanoski;L. Köpke;C. Kopper;S. Kopper;D. Koskinen;M. Kowalski;K. Krings;M. Kroll;G. Krückl;S. Kunwar;N. Kurahashi;A. Kyriacou;M. Labare;J. Lanfranchi;M. Larson;F. Lauber;K. Leonard;M. Leuermann;Q. Liu;E. Lohfink;C. J. L. Mariscal;L. Lu;J. Lünemann;W. Luszczak;J. Madsen;G. Maggi;K. Mahn;Y. Makino;S. Mancina;I. Mariş;R. Maruyama;K. Mase;R. Maunu;K. Meagher;M. Medici;M. Meier;T. Menne;G. Merino;T. Meures;S. Miarecki;J. Micallef;G. Momenté;T. Montaruli;R. Moore;M. Moulai;R. Nagai;R. Nahnhauer;P. Nakarmi;U. Naumann;G. Neer;H. Niederhausen;S. Nowicki;D. Nygren;A. Obertacke Pollmann;A. Olivas;A. O'Murchadha;E. O’Sullivan;T. Palczewski;H. Pandya;D. Pankova;P. Peiffer;C. Pérez de los Heros;D. Pieloth;E. Pinat;A. Pizzuto;M. Plum;P. Price;G. Przybylski;C. Raab;M. Rameez;L. Rauch;K. Rawlins;I. C. Rea;R. Reimann;B. Relethford;G. Renzi;E. Resconi;W. Rhode;M. Richman;S. Robertson;M. Rongen;C. Rott;T. Ruhe;D. Ryckbosch;D. Rysewyk;I. Safa;S. Sanchez Herrera;A. Sandrock;J. Sandroos;M. Santander;S. Sarkar;K. Satalecka;M. Schaufel;P. Schlunder;T. Schmidt;A. Schneider;J. Schneider;S. Schöneberg;L. Schumacher;S. Sclafani;D. Seckel;S. Seunarine;J. Soedingrekso;D. Soldin;M. Song;G. Spiczak;C. Spiering;J. Stachurska;M. Stamatikos;T. Stanev;Alexander Stasik;R. Stein;J. Stettner;A. Steuer;T. Stezelberger;R. Stokstad;A. Stößl;N. Strotjohann;T. Stuttard;G. Sullivan;M. Sutherland;I. Taboada;F. Tenholt;S. Ter-Antonyan;A. Terliuk;S. Tilav;M. Tobin;C. Tönnis;S. Toscano;D. Tosi;M. Tselengidou;C. Tung;A. Turcati;R. Turcotte;C. Turley;B. Ty;E. Unger;M. U. Unland Elorrieta;M. Usner;J. Vandenbroucke;W. Driessche;D. Eijk;N. Eijndhoven;S. Vanheule;J. Santen;M. Vraeghe;C. Walck;A. Wallace;M. Wallraff;F. Wandler;N. Wandkowsky;T. B. Watson;C. Weaver;M. Weiss;C. Wendt;J. Werthebach;S. Westerhoff;B. Whelan;N. Whitehorn;K. Wiebe;C. Wiebusch;L. Wille;D. Williams;L. Wills;M. Wolf;J. Wood;T. R. Wood;E. Woolsey;K. Woschnagg;G. Wrede;D. Xu;X. Xu;Y. Xu;J. Yáñez;G. Yodh;S. Yoshida;T. Yuan;I. Collaboration
中科院分区：
文献类型：
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作者：
M. Aartsen;M. Ackermann;J. Adams;J. Aguilar;M. Ahlers;M. Ahrens;D. Altmann;K. Andeen;T. Anderson;I. Ansseau;G. Anton;C. Argüelles;J. Auffenberg;S. Axani;P. Backes;H. Bagherpour;X. Bai;A. Barbano;J. P. Barron;S. Barwick;V. Baum;R. Bay;J. Beatty;J. Becker Tjus;K. Becker;S. BenZvi;D. Berley;E. Bernardini;D. Besson;G. Binder;D. Bindig;E. Blaufuss;S. Blot;C. Bohm;M. Börner;F. Bos;S. Böser;O. Botner;E. Bourbeau;J. Bourbeau;F. Bradascio;J. Braun;H. Bretz;S. Bron;J. Brostean-Kaiser;A. Burgman;R. Busse;T. Carver;C. Chen;E. Cheung;D. Chirkin;K. Clark;L. Classen;G. Collin;J. Conrad;P. Coppin;P. Correa;D. Cowen;R. Cross;P. Dave;M. Day;J. D. André;C. Clercq;J. DeLaunay;H. Dembinski;K. Deoskar;S. Ridder;P. Desiati;K. D. Vries;G. Wasseige;M. With;T. DeYoung;J. C. Díaz-Vélez;H. Dujmovic;M. Dunkman;E. Dvorak;B. Eberhardt;T. Ehrhardt;B. Eichmann;P. Eller;P. Evenson;S. Fahey;A. Fazely;J. Felde;K. Filimonov;C. Finley;A. Franckowiak;E. Friedman;A. Fritz;T. Gaisser;J. Gallagher;E. Ganster;S. Garrappa;L. Gerhardt;K. Ghorbani;W. Giang;T. Glauch;T. Glüsenkamp;A. Goldschmidt;J. G. Gonzalez;D. Grant;Z. Griffith;C. Haack;A. Hallgren;L. Halve;F. Halzen;K. Hanson;D. Hebecker;D. Heereman;K. Helbing;R. Hellauer;S. Hickford;J. Hignight;G. Hill;K. Hoffman;R. Hoffmann;T. Hoinka;B. Hokanson-Fasig;K. Hoshina;F. Huang;M. Huber;K. Hultqvist;Mirco Hünnefeld;R. Hussain;S. In;N. Iovine;A. Ishihara;E. Jacobi;G. Japaridze;M. Jeong;K. Jero;B. Jones;P. Kalaczyński;W. Kang;A. Kappes;D. Kappesser;T. Karg;A. Karle;U. Katz;M. Kauer;A. Keivani;J. Kelley;A. Kheirandish;J. Kim;T. Kintscher;J. Kiryluk;T. Kittler;S. Klein;R. Koirala;H. Kolanoski;L. Köpke;C. Kopper;S. Kopper;D. Koskinen;M. Kowalski;K. Krings;M. Kroll;G. Krückl;S. Kunwar;N. Kurahashi;A. Kyriacou;M. Labare;J. Lanfranchi;M. Larson;F. Lauber;K. Leonard;M. Leuermann;Q. Liu;E. Lohfink;C. J. L. Mariscal;L. Lu;J. Lünemann;W. Luszczak;J. Madsen;G. Maggi;K. Mahn;Y. Makino;S. Mancina;I. Mariş;R. Maruyama;K. Mase;R. Maunu;K. Meagher;M. Medici;M. Meier;T. Menne;G. Merino;T. Meures;S. Miarecki;J. Micallef;G. Momenté;T. Montaruli;R. Moore;M. Moulai;R. Nagai;R. Nahnhauer;P. Nakarmi;U. Naumann;G. Neer;H. Niederhausen;S. Nowicki;D. Nygren;A. Obertacke Pollmann;A. Olivas;A. O'Murchadha;E. O’Sullivan;T. Palczewski;H. Pandya;D. Pankova;P. Peiffer;C. Pérez de los Heros;D. Pieloth;E. Pinat;A. Pizzuto;M. Plum;P. Price;G. Przybylski;C. Raab;M. Rameez;L. Rauch;K. Rawlins;I. C. Rea;R. Reimann;B. Relethford;G. Renzi;E. Resconi;W. Rhode;M. Richman;S. Robertson;M. Rongen;C. Rott;T. Ruhe;D. Ryckbosch;D. Rysewyk;I. Safa;S. Sanchez Herrera;A. Sandrock;J. Sandroos;M. Santander;S. Sarkar;K. Satalecka;M. Schaufel;P. Schlunder;T. Schmidt;A. Schneider;J. Schneider;S. Schöneberg;L. Schumacher;S. Sclafani;D. Seckel;S. Seunarine;J. Soedingrekso;D. Soldin;M. Song;G. Spiczak;C. Spiering;J. Stachurska;M. Stamatikos;T. Stanev;Alexander Stasik;R. Stein;J. Stettner;A. Steuer;T. Stezelberger;R. Stokstad;A. Stößl;N. Strotjohann;T. Stuttard;G. Sullivan;M. Sutherland;I. Taboada;F. Tenholt;S. Ter-Antonyan;A. Terliuk;S. Tilav;M. Tobin;C. Tönnis;S. Toscano;D. Tosi;M. Tselengidou;C. Tung;A. Turcati;R. Turcotte;C. Turley;B. Ty;E. Unger;M. U. Unland Elorrieta;M. Usner;J. Vandenbroucke;W. Driessche;D. Eijk;N. Eijndhoven;S. Vanheule;J. Santen;M. Vraeghe;C. Walck;A. Wallace;M. Wallraff;F. Wandler;N. Wandkowsky;T. B. Watson;C. Weaver;M. Weiss;C. Wendt;J. Werthebach;S. Westerhoff;B. Whelan;N. Whitehorn;K. Wiebe;C. Wiebusch;L. Wille;D. Williams;L. Wills;M. Wolf;J. Wood;T. R. Wood;E. Woolsey;K. Woschnagg;G. Wrede;D. Xu;X. Xu;Y. Xu;J. Yáñez;G. Yodh;S. Yoshida;T. Yuan;I. Collaboration
冰立方合作组观测到一个高能天体物理中微子流，最近发现了耀变体TXS 0506+ 056的中微子发射证据。这些结果为高能宇宙打开了一扇新的窗户。然而，大多数观测到的天体物理中微子流的来源仍然不确定。在这里，稳定的点状中微子源的搜索是使用未分组的似然分析。该方法使用IceCube在2009年至2017年期间记录的约497，000个中微子的非常高的统计样本来搜索μ子中微子事件的空间积累。在1 TeV时，中值角分辨率为1.1 μ m，并提高到1.0 μ m。对于能量为1 PeV的中微子，为3 μ s。与以前的分析相比，这种搜索是优化的点状中微子发射与观测到的天体物理学μ介子中微子通量相同的通量特性，并介绍了改进的事件重建和参数化的背景。结果是，与之前假设E− 2谱的分析相比，μ子-中微子通量的灵敏度提高了35%。对μ介子-中微子通量的灵敏度为E2 dN/dE= 3· 10− 13 TeV cm− 2 s− 1。在全天扫描和由伽马射线观测激发的先验候选源列表中没有发现中微子源的新证据。此外，没有显着的过量以上的背景下，发现从人口的阈值源。潜在的源类的非观测的影响进行了讨论。
Abstract The IceCube Collaboration has observed a highenergy astrophysical neutrino flux and recently found evidence for neutrino emission from the blazar TXS 0506+ 056. These results open a new window into the high-energy universe. However, the source or sources of most of the observed flux of astrophysical neutrinos remains uncertain. Here, a search for steady point-like neutrino sources is performed using an unbinned likelihood analysis. The method searches for a spatial accumulation of muon-neutrino events using the very high-statistics sample of about 497,000 neutrinos recorded by IceCube between 2009 and 2017. The median angular resolution is∼ 1◦ at 1 TeV and improves to∼ 0. 3◦ for neutrinos with an energy of 1 PeV. Compared to previous analyses, this search is optimized for point-like neutrino emission with the same flux-characteristics as the observed astrophysical muon-neutrino flux and introduces an improved event-reconstruction and parametrization of the background. The result is an improvement in sensitivity to the muon-neutrino flux compared to the previous analysis of∼ 35% assuming an E− 2 spectrum. The sensitivity on the muon-neutrino flux is at a level of E2dN/dE= 3· 10− 13 TeV cm− 2 s− 1. No new evidence for neutrino sources is found in a full sky scan and in an a priori candidate source list that is motivated by gamma-ray observations. Furthermore, no significant excesses above background are found from populations of sub-threshold sources. The implications of the non-observation for potential source classes are discussed.