Constraints on Galactic Neutrino Emission with Seven Years of IceCube Data
Constraints on Galactic Neutrino Emission with Seven Years of IceCube Data
复制标题
DOI：
10.3847/1538-4357/aa8dfb
复制
发表时间：
2017-07
期刊：
影响因子：
--
通讯作者：
I. C. M. Aartsen;M. Ackermann;J. Adams;J. Aguilar;M. Ahlers;M. Ahrens;I. A. Samarai;D. Altmann;K. Andeen;T. Anderson;I. Ansseau;G. Anton;C. Arguelles;J. Auffenberg;S. Axani;H. Bagherpour;X. Bai;J. P. Barron;S. Barwick;V. Baum;R. Bay;J. Beatty;J. Tjus;K. Becker;S. BenZvi;D. Berley;E. Bernardini;D. Besson;G. Binder;D. Bindig;E. Blaufuss;S. Blot;C. Bohm;M. Borner;F. Bos;D. Bose;S. Boser;O. Botner;J. Bourbeau;F. Bradascio;J. Braun;L. Brayeur;M. Brenzke;H. Bretz;S. Bron;A. Burgman;T. Carver;J. Casey;M. Casier;E. Cheung;D. Chirkin;A. Christov;K. Clark;L. Classen;S. Coenders;G. Collin;J. Conrad;D. Cowen;R. Cross;M. Day;J. Andr'e;C. Clercq;J. DeLaunay;H. Dembinski;S. Ridder;P. Desiati;K. D. Vries;G. Wasseige;M. With;T. DeYoung;J. C. D'iaz-V'elez;V. Lorenzo;H. Dujmovic;J. Dumm;M. Dunkman;B. Eberhardt;T. Ehrhardt;B. Eichmann;P. Eller;P. Evenson;S. Fahey;A. Fazely;J. Felde;K. Filimonov;C. Finley;S. Flis;A. Franckowiak;E. Friedman;T. Fuchs;T. Gaisser;J. Gallagher;L. Gerhardt;K. Ghorbani;W. Giang;T. Glauch;T. Glusenkamp;A. Goldschmidt;J. G. Gonzalez;D. Grant;Z. Griffith;C. Haack;A. Hallgren;F. Halzen;K. Hanson;D. Hebecker;D. Heereman;K. Helbing;R. Hellauer;S. Hickford;J. Hignight;G. Hill;K. Hoffman;R. Hoffmann;B. Hokanson-Fasig;K. Hoshina;F. Huang;M. Huber;K. Hultqvist;S. In;A. Ishihara;E. Jacobi;G. Japaridze;M. Jeong;K. Jero;B. Jones;P. Kalacynski;W. Kang;A. Kappes;T. Karg;A. Karle;U. Katz;M. Kauer;A. Keivani;J. Kelley;A. Kheirandish;J. Kim;M. Kim;T. Kintscher;J. Kiryluk;T. Kittler;S. Klein;G. Kohnen;R. Koirala;H. Kolanoski;L. Kopke;C. Kopper;S. Kopper;J. Koschinsky;D. Koskinen;M. Kowalski;K. Krings;M. Kroll;G. Kruckl;J. Kunnen;S. Kunwar;N. Kurahashi;T. Kuwabara;A. Kyriacou;M. Labare;J. Lanfranchi;M. Larson;F. Lauber;D. Lennarz;M. Lesiak-Bzdak;M. Leuermann;Q. Liu;L. Lu;J. Lunemann;W. Luszczak;J. Madsen;G. Maggi;K. Mahn;S. Mancina;R. Maruyama;K. Mase;R. Maunu;F. McNally;K. Meagher;M. Medici;M. Meier;T. Menne;G. Merino;T. Meures;S. Miarecki;J. Micallef;G. Moment'e;T. Montaruli;R. Moore;M. Moulai;R. Nahnhauer;P. Nakarmi;U. Naumann;G. Neer;H. Niederhausen;S. Nowicki;D. Nygren;A. Pollmann;A. Olivas;A. O'Murchadha;T. Palczewski;H. Pandya;D. Pankova;P. Peiffer;J. Pepper;C. Heros;D. Pieloth;E. Pinat;M. Plum;P. Price;G. Przybylski;C. Raab;L. Radel;M. Rameez;K. Rawlins;R. Reimann;B. Relethford;M. Relich;E. Resconi;W. Rhode;M. Richman;S. Robertson;M. Rongen;C. Rott;T. Ruhe;D. Ryckbosch;D. Rysewyk;T. Salzer;S. Herrera;A. Sandrock;J. Sandroos;S. Sarkar;K. Satalecka;P. Schlunder;T. Schmidt;A. Schneider;S. Schoenen;S. Schoneberg;L. Schumacher;D. Seckel;S. Seunarine;D. Soldin;M. Song;G. Spiczak;C. Spiering;J. Stachurska;T. Stanev;Alexander Stasik;J. Stettner;A. Steuer;T. Stezelberger;R. Stokstad;A. Stossl;N. Strotjohann;G. Sullivan;M. Sutherland;I. Taboada;J. Tatar;F. Tenholt;S. Ter-Antonyan;A. Terliuk;G. Tevsi'c;S. Tilav;P. Toale;M. Tobin;S. Toscano;D. Tosi;M. Tselengidou;C. Tung;A. Turcati;C. Turley;B. Ty;E. Unger;M. Usner;J. Vandenbroucke;W. Driessche;N. Eijndhoven;S. Vanheule;J. Santen;M. Vehring;E. Vogel;M. Vraeghe;C. Walck;A. Wallace;M. Wallraff;F. Wandler;N. Wandkowsky;A. Waza;C. Weaver;M. Weiss;C. Wendt;S. Westerhoff;B. Whelan;S. Wickmann;K. Wiebe;C. Wiebusch;L. Wille;D. Williams;L. Wills;M. Wolf;J. Wood;T. R. Wood;E. Woolsey;K. Woschnagg;D. Xu;X. Xu;Y. Xu;J. Yáñez;G. Yodh;S. Yoshida;T. Yuan;M. Zoll
中科院分区：
文献类型：
--
作者：
I. C. M. Aartsen;M. Ackermann;J. Adams;J. Aguilar;M. Ahlers;M. Ahrens;I. A. Samarai;D. Altmann;K. Andeen;T. Anderson;I. Ansseau;G. Anton;C. Arguelles;J. Auffenberg;S. Axani;H. Bagherpour;X. Bai;J. P. Barron;S. Barwick;V. Baum;R. Bay;J. Beatty;J. Tjus;K. Becker;S. BenZvi;D. Berley;E. Bernardini;D. Besson;G. Binder;D. Bindig;E. Blaufuss;S. Blot;C. Bohm;M. Borner;F. Bos;D. Bose;S. Boser;O. Botner;J. Bourbeau;F. Bradascio;J. Braun;L. Brayeur;M. Brenzke;H. Bretz;S. Bron;A. Burgman;T. Carver;J. Casey;M. Casier;E. Cheung;D. Chirkin;A. Christov;K. Clark;L. Classen;S. Coenders;G. Collin;J. Conrad;D. Cowen;R. Cross;M. Day;J. Andr'e;C. Clercq;J. DeLaunay;H. Dembinski;S. Ridder;P. Desiati;K. D. Vries;G. Wasseige;M. With;T. DeYoung;J. C. D'iaz-V'elez;V. Lorenzo;H. Dujmovic;J. Dumm;M. Dunkman;B. Eberhardt;T. Ehrhardt;B. Eichmann;P. Eller;P. Evenson;S. Fahey;A. Fazely;J. Felde;K. Filimonov;C. Finley;S. Flis;A. Franckowiak;E. Friedman;T. Fuchs;T. Gaisser;J. Gallagher;L. Gerhardt;K. Ghorbani;W. Giang;T. Glauch;T. Glusenkamp;A. Goldschmidt;J. G. Gonzalez;D. Grant;Z. Griffith;C. Haack;A. Hallgren;F. Halzen;K. Hanson;D. Hebecker;D. Heereman;K. Helbing;R. Hellauer;S. Hickford;J. Hignight;G. Hill;K. Hoffman;R. Hoffmann;B. Hokanson-Fasig;K. Hoshina;F. Huang;M. Huber;K. Hultqvist;S. In;A. Ishihara;E. Jacobi;G. Japaridze;M. Jeong;K. Jero;B. Jones;P. Kalacynski;W. Kang;A. Kappes;T. Karg;A. Karle;U. Katz;M. Kauer;A. Keivani;J. Kelley;A. Kheirandish;J. Kim;M. Kim;T. Kintscher;J. Kiryluk;T. Kittler;S. Klein;G. Kohnen;R. Koirala;H. Kolanoski;L. Kopke;C. Kopper;S. Kopper;J. Koschinsky;D. Koskinen;M. Kowalski;K. Krings;M. Kroll;G. Kruckl;J. Kunnen;S. Kunwar;N. Kurahashi;T. Kuwabara;A. Kyriacou;M. Labare;J. Lanfranchi;M. Larson;F. Lauber;D. Lennarz;M. Lesiak-Bzdak;M. Leuermann;Q. Liu;L. Lu;J. Lunemann;W. Luszczak;J. Madsen;G. Maggi;K. Mahn;S. Mancina;R. Maruyama;K. Mase;R. Maunu;F. McNally;K. Meagher;M. Medici;M. Meier;T. Menne;G. Merino;T. Meures;S. Miarecki;J. Micallef;G. Moment'e;T. Montaruli;R. Moore;M. Moulai;R. Nahnhauer;P. Nakarmi;U. Naumann;G. Neer;H. Niederhausen;S. Nowicki;D. Nygren;A. Pollmann;A. Olivas;A. O'Murchadha;T. Palczewski;H. Pandya;D. Pankova;P. Peiffer;J. Pepper;C. Heros;D. Pieloth;E. Pinat;M. Plum;P. Price;G. Przybylski;C. Raab;L. Radel;M. Rameez;K. Rawlins;R. Reimann;B. Relethford;M. Relich;E. Resconi;W. Rhode;M. Richman;S. Robertson;M. Rongen;C. Rott;T. Ruhe;D. Ryckbosch;D. Rysewyk;T. Salzer;S. Herrera;A. Sandrock;J. Sandroos;S. Sarkar;K. Satalecka;P. Schlunder;T. Schmidt;A. Schneider;S. Schoenen;S. Schoneberg;L. Schumacher;D. Seckel;S. Seunarine;D. Soldin;M. Song;G. Spiczak;C. Spiering;J. Stachurska;T. Stanev;Alexander Stasik;J. Stettner;A. Steuer;T. Stezelberger;R. Stokstad;A. Stossl;N. Strotjohann;G. Sullivan;M. Sutherland;I. Taboada;J. Tatar;F. Tenholt;S. Ter-Antonyan;A. Terliuk;G. Tevsi'c;S. Tilav;P. Toale;M. Tobin;S. Toscano;D. Tosi;M. Tselengidou;C. Tung;A. Turcati;C. Turley;B. Ty;E. Unger;M. Usner;J. Vandenbroucke;W. Driessche;N. Eijndhoven;S. Vanheule;J. Santen;M. Vehring;E. Vogel;M. Vraeghe;C. Walck;A. Wallace;M. Wallraff;F. Wandler;N. Wandkowsky;A. Waza;C. Weaver;M. Weiss;C. Wendt;S. Westerhoff;B. Whelan;S. Wickmann;K. Wiebe;C. Wiebusch;L. Wille;D. Williams;L. Wills;M. Wolf;J. Wood;T. R. Wood;E. Woolsey;K. Woschnagg;D. Xu;X. Xu;Y. Xu;J. Yáñez;G. Yodh;S. Yoshida;T. Yuan;M. Zoll
尽管人们广泛寻找高能天体物理中微子的来源，但其起源仍然是个谜。我们提出了来自 IceCube 中微子观测站七年的 μ 子数据对来自银河平面的中微子通量的限制。这种通量预计来自宇宙射线与星际介质或附近局部源的相互作用。开发了两种方法来测试整个平面的空间扩展通量，这两种方法都是最大似然拟合，但采用不同的信号和背景建模技术。我们考虑主要基于伽马射线观测和涵盖广泛可能性的模型的银河中微子发射的三个模板。基于这些模板以及在未破坏的 E-2.5 幂律能谱的基准情况下，我们设置了 90% 的置信度上限，将银河系对弥散中微子通量的可能贡献限制在相对较小的范围内，小于 Aartsen 等人报告的通量的 14%。高于 1 TeV。堆叠方法也用于测试已知高能银河伽马射线源的目录。
The origins of high-energy astrophysical neutrinos remain a mystery despite extensive searches for their sources. We present constraints from seven years of IceCube Neutrino Observatory muon data on the neutrino flux coming from the Galactic plane. This flux is expected from cosmic-ray interactions with the interstellar medium or near localized sources. Two methods were developed to test for a spatially extended flux from the entire plane, both of which are maximum likelihood fits but with different signal and background modeling techniques. We consider three templates for Galactic neutrino emission based primarily on gamma-ray observations and models that cover a wide range of possibilities. Based on these templates and in the benchmark case of an unbroken E − 2.5 power-law energy spectrum, we set 90% confidence level upper limits, constraining the possible Galactic contribution to the diffuse neutrino flux to be relatively small, less than 14% of the flux reported in Aartsen et al. above 1 TeV. A stacking method is also used to test catalogs of known high-energy Galactic gamma-ray sources.