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Constraints on Galactic Neutrino Emission with Seven Years of IceCube Data

  • M. G. Aartsen
  • , M. Ackermann
  • , J. Adams
  • , J. A. Aguilar
  • , M. Ahlers
  • , M. Ahrens
  • , I. Al Samarai
  • , D. Altmann
  • , K. Andeen
  • , T. Anderson
  • , I. Ansseau
  • , G. Anton
  • , C. Argüelles
  • , J. Auffenberg
  • , S. Axani
  • , H. Bagherpour
  • , X. Bai
  • , J. P. Barron
  • , S. W. Barwick
  • , V. Baum
  • R. Bay, J. J. Beatty, J. Becker Tjus, K. H. Becker, S. Benzvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, C. Bohm, M. Börner, F. Bos, D. Bose, S. Böser, O. Botner, J. Bourbeau, F. Bradascio, J. Braun, L. Brayeur, M. Brenzke, H. P. Bretz, S. Bron, A. Burgman, T. Carver, J. Casey, M. Casier, E. Cheung, D. Chirkin, A. Christov, K. Clark, L. Classen, S. Coenders, G. H. Collin, J. M. Conrad, D. F. Cowen, R. Cross, M. Day, J. P.A.M.D. André, C. De Clercq, J. J. Delaunay, H. Dembinski, S. De Ridder, P. Desiati, K. D.De Vries, G. De Wasseige, M. De With, T. Deyoung, J. C. Daz-Vélez, V. Di Lorenzo, H. Dujmovic, J. P. Dumm, M. Dunkman, B. Eberhardt, T. Ehrhardt, B. Eichmann, P. Eller, P. A. Evenson, S. Fahey, A. R. Fazely, J. Felde, K. Filimonov, C. Finley, S. Flis, A. Franckowiak, E. Friedman, T. Fuchs, T. K. Gaisser, J. Gallagher, L. Gerhardt, K. Ghorbani, W. Giang, T. Glauch, T. Glüsenkamp, 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. C. Hill, K. D. Hoffman, R. Hoffmann, B. Hokanson-Fasig, K. Hoshina, F. Huang, M. Huber, K. Hultqvist, S. In, A. Ishihara, E. Jacobi, G. S. Japaridze, M. Jeong, K. Jero, B. J.P. Jones, P. Kalacynski, W. Kang, A. Kappes, T. Karg, A. Karle, U. Katz, M. Kauer, A. Keivani, J. L. Kelley, A. Kheirandish, J. Kim, M. Kim, T. Kintscher, J. Kiryluk, T. Kittler, S. R. Klein, G. Kohnen, R. Koirala, H. Kolanoski, L. Köpke, C. Kopper, S. Kopper, J. P. Koschinsky, D. J. Koskinen, M. Kowalski, K. Krings, M. Kroll, G. Krückl, J. Kunnen, S. Kunwar, N. Kurahashi, T. Kuwabara, A. Kyriacou, M. Labare, J. L. Lanfranchi, M. J. Larson, F. Lauber, D. Lennarz, M. Lesiak-Bzdak, M. Leuermann, Q. R. Liu, L. Lu, J. Lünemann, W. Luszczak, J. Madsen, G. Maggi, K. B.M. 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. Momenté, T. Montaruli, R. W. Moore, M. Moulai, R. Nahnhauer, P. Nakarmi, U. Naumann, G. Neer, H. Niederhausen, S. C. Nowicki, D. R. Nygren, A. Obertacke Pollmann, A. Olivas, A. O'Murchadha, T. Palczewski, H. Pandya, D. V. Pankova, P. Peiffer, J. A. Pepper, C. Pérez De Los Heros, D. Pieloth, E. Pinat, M. Plum, P. B. Price, G. T. 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. E.Sanchez Herrera, A. Sandrock, J. Sandroos, S. Sarkar, K. Satalecka, P. Schlunder, T. Schmidt, A. Schneider, S. Schoenen, S. Schöneberg, L. Schumacher, D. Seckel, S. Seunarine, D. Soldin, M. Song, G. M. Spiczak, C. Spiering, J. Stachurska, T. Stanev, A. Stasik, J. Stettner, A. Steuer, T. Stezelberger, R. G. Stokstad, A. Stößl, N. L. Strotjohann, G. W. Sullivan, M. Sutherland, I. Taboada, J. Tatar, F. Tenholt, S. Ter-Antonyan, A. Terliuk, G. Tešić, S. Tilav, P. A. Toale, M. N. Tobin, S. Toscano, D. Tosi, M. Tselengidou, C. F. Tung, A. Turcati, C. F. Turley, B. Ty, E. Unger, M. Usner, J. Vandenbroucke, W. Van Driessche, N. Van Eijndhoven, S. Vanheule, J. Van Santen, M. Vehring, E. Vogel, M. Vraeghe, C. Walck, A. Wallace, M. Wallraff, F. D. Wandler, N. Wandkowsky, A. Waza, C. Weaver, M. J. Weiss, C. Wendt, S. Westerhoff, B. J. Whelan, S. Wickmann, K. Wiebe, C. H. Wiebusch, L. Wille, D. R. Williams, L. Wills, M. Wolf, J. Wood, T. R. Wood, E. Woolsey, K. Woschnagg, D. L. Xu, X. W. Xu, Y. Xu, J. P. Yanez, G. Yodh, S. Yoshida, T. Yuan, M. Zoll
  • University of Adelaide
  • German Electron Synchrotron
  • University of Canterbury
  • Université libre de Bruxelles
  • University of Copenhagen
  • Stockholm University
  • University of Geneva
  • Friedrich-Alexander University Erlangen-Nürnberg
  • Marquette University
  • Pennsylvania State University
  • Massachusetts Institute of Technology
  • RWTH Aachen University
  • South Dakota School of Mines & Technology
  • University of Alberta
  • University of California at Irvine
  • Johannes Gutenberg University Mainz
  • University of California at Berkeley
  • Ohio State University
  • Ruhr University Bochum
  • University of Wuppertal
  • University of Rochester
  • University of Maryland, College Park
  • University of Kansas
  • Lawrence Berkeley National Laboratory
  • TU Dortmund University
  • Sungkyunkwan University
  • Uppsala University
  • University of Wisconsin-Madison
  • Vrije Universiteit Brussel
  • SNOLAB
  • University of Münster
  • Technical University of Munich
  • Michigan State University
  • University of Delaware
  • Ghent University
  • Humboldt University of Berlin
  • Southern University and A&M College
  • The University of Tokyo
  • Chiba University
  • Clark Atlanta University
  • University of Texas at Arlington
  • Universite de Mons
  • University of Alabama
  • Drexel University
  • Stony Brook University
  • University of Wisconsin-River Falls
  • Yale University
  • University of Alaska Anchorage
  • University of Oxford
  • Georgia Institute of Technology

Research output: Contribution to journalArticlepeer-review

132 Scopus citations

Abstract

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.

Original languageEnglish
Article number67
JournalAstrophysical Journal
Volume849
Issue number1
DOIs
StatePublished - Nov 1 2017

Keywords

  • gamma rays: ISM

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