利用七年 IceCube 数据对银河系中微子发射的限制
高能天体物理现象
2017-11-08 v1
摘要
尽管进行了广泛的源搜索，高能天体物理中微子的起源仍然是一个谜。我们展示了基于七年 IceCube 中微子天文台缪子数据，对来自银河系平面的中微子通量的限制。预计该通量来自宇宙射线与星际介质的相互作用或靠近局部源。开发了两种方法来测试来自整个平面的空间扩展通量，两者均为最大似然拟合，但采用了不同的信号和背景建模技术。我们考虑了主要基于伽马射线观测和模型的三种银河系中微子发射模板，涵盖了广泛的可能性。基于这些模板和未折断的 幂律能谱，我们设定了 90% 置信水平的上限，限制可能的银河系贡献占弥漫中微子通量的比例相对较小，在 1 TeV 以上小于 Aartsen 等人 (2015a) 报告通量的 14%。还使用堆叠方法测试了已知高能银河系伽马射线源的星表。
引用
@article{arxiv.1707.03416,
title = {Constraints on Galactic Neutrino Emission with Seven Years of IceCube Data},
author = {IceCube Collaboration and M. G. Aartsen and M. Ackermann and J. Adams and J. A. Aguilar and M. Ahlers and M. Ahrens and I. Al Samarai and D. Altmann and K. Andeen and T. Anderson and I. Ansseau and G. Anton and C. Argüelles and J. Auffenberg and S. Axani and H. Bagherpour and X. Bai and J. P. Barron and S. W. Barwick and V. Baum and R. Bay and J. J. Beatty and J. Becker Tjus and K. -H. Becker and S. BenZvi and D. Berley and E. Bernardini and D. Z. Besson and G. Binder and D. Bindig and E. Blaufuss and S. Blot and C. Bohm and M. Börner and F. Bos and D. Bose and S. Böser and O. Botner and J. Bourbeau and F. Bradascio and J. Braun and L. Brayeur and M. Brenzke and H. -P. Bretz and S. Bron and A. Burgman and T. Carver and J. Casey and M. Casier and E. Cheung and D. Chirkin and A. Christov and K. Clark and L. Classen and S. Coenders and G. H. Collin and J. M. Conrad and D. F. Cowen and R. Cross and M. Day and J. P. A. M. de André and C. De Clercq and J. J. DeLaunay and H. Dembinski and S. De Ridder and P. Desiati and K. D. de Vries and G. de Wasseige and M. de With and T. DeYoung and J. C. Díaz-Vélez and V. di Lorenzo and H. Dujmovic and J. P. Dumm and M. Dunkman and B. Eberhardt and T. Ehrhardt and B. Eichmann and P. Eller and P. A. Evenson and S. Fahey and A. R. Fazely and J. Felde and K. Filimonov and C. Finley and S. Flis and A. Franckowiak and E. Friedman and T. Fuchs and T. K. Gaisser and J. Gallagher and L. Gerhardt and K. Ghorbani and W. Giang and T. Glauch and T. Glüsenkamp and A. Goldschmidt and J. G. Gonzalez and D. Grant and Z. Griffith and C. Haack and A. Hallgren and F. Halzen and K. Hanson and D. Hebecker and D. Heereman and K. Helbing and R. Hellauer and S. Hickford and J. Hignight and G. C. Hill and K. D. Hoffman and R. Hoffmann and B. Hokanson-Fasig and K. Hoshina and F. Huang and M. Huber and K. Hultqvist and S. In and A. Ishihara and E. Jacobi and G. S. Japaridze and M. Jeong and K. Jero and B. J. P. Jones and P. Kalacynski and W. Kang and A. Kappes and T. Karg and A. Karle and U. Katz and M. Kauer and A. Keivani and J. L. Kelley and A. Kheirandish and J. Kim and M. Kim and T. Kintscher and J. Kiryluk and T. Kittler and S. R. Klein and G. Kohnen and R. Koirala and H. Kolanoski and L. Köpke and C. Kopper and S. Kopper and J. P. Koschinsky and D. J. Koskinen and M. Kowalski and K. Krings and M. Kroll and G. Krückl and J. Kunnen and S. Kunwar and N. Kurahashi and T. Kuwabara and A. Kyriacou and M. Labare and J. L. Lanfranchi and M. J. Larson and F. Lauber and D. Lennarz and M. Lesiak-Bzdak and M. Leuermann and Q. R. Liu and L. Lu and J. Lünemann and W. Luszczak and J. Madsen and G. Maggi and K. B. M. Mahn and S. Mancina and R. Maruyama and K. Mase and R. Maunu and F. McNally and K. Meagher and M. Medici and M. Meier and T. Menne and G. Merino and T. Meures and S. Miarecki and J. Micallef and G. Momenté and T. Montaruli and R. W. Moore and M. Moulai and R. Nahnhauer and P. Nakarmi and U. Naumann and G. Neer and H. Niederhausen and S. C. Nowicki and D. R. Nygren and A. Obertacke Pollmann and A. Olivas and A. O'Murchadha and T. Palczewski and H. Pandya and D. V. Pankova and P. Peiffer and J. A. Pepper and C. Pérez de los Heros and D. Pieloth and E. Pinat and M. Plum and P. B. Price and G. T. Przybylski and C. Raab and L. Rädel and M. Rameez and K. Rawlins and R. Reimann and B. Relethford and M. Relich and E. Resconi and W. Rhode and M. Richman and S. Robertson and M. Rongen and C. Rott and T. Ruhe and D. Ryckbosch and D. Rysewyk and T. Sälzer and S. E. Sanchez Herrera and A. Sandrock and J. Sandroos and S. Sarkar and S. Sarkar and K. Satalecka and P. Schlunder and T. Schmidt and A. Schneider and S. Schoenen and S. Schöneberg and L. Schumacher and D. Seckel and S. Seunarine and D. Soldin and M. Song and G. M. Spiczak and C. Spiering and J. Stachurska and T. Stanev and A. Stasik and J. Stettner and A. Steuer and T. Stezelberger and R. G. Stokstad and A. Stößl and N. L. Strotjohann and G. W. Sullivan and M. Sutherland and I. Taboada and J. Tatar and F. Tenholt and S. Ter-Antonyan and A. Terliuk and G. Tešić and S. Tilav and P. A. Toale and M. N. Tobin and S. Toscano and D. Tosi and M. Tselengidou and C. F. Tung and A. Turcati and C. F. Turley and B. Ty and E. Unger and M. Usner and J. Vandenbroucke and W. Van Driessche and N. van Eijndhoven and S. Vanheule and J. van Santen and M. Vehring and E. Vogel and M. Vraeghe and C. Walck and A. Wallace and M. Wallraff and F. D. Wandler and N. Wandkowsky and A. Waza and C. Weaver and M. J. Weiss and C. Wendt and S. Westerhoff and B. J. Whelan and S. Wickmann and K. Wiebe and C. H. Wiebusch and L. Wille and D. R. Williams and L. Wills and M. Wolf and J. Wood and T. R. Wood and E. Woolsey and K. Woschnagg and D. L. Xu and X. W. Xu and Y. Xu and J. P. Yanez and G. Yodh and S. Yoshida and T. Yuan and M. Zoll},
journal= {arXiv preprint arXiv:1707.03416},
year = {2017}
}
备注
14 pages, 4 figures, 4 tables, submitted to The Astrophysical Journal