dc.contributor.author | Kachelriess, Michael | |
dc.contributor.author | Neronov, Andrii Yu. | |
dc.contributor.author | Semikoz, Dimitry V. | |
dc.date.accessioned | 2020-01-16T07:09:12Z | |
dc.date.available | 2020-01-16T07:09:12Z | |
dc.date.created | 2019-08-13T13:52:13Z | |
dc.date.issued | 2019 | |
dc.identifier.citation | Journal of Physics: Conference Series. 2019, 1181 (1), 1-6. | nb_NO |
dc.identifier.issn | 1742-6588 | |
dc.identifier.uri | http://hdl.handle.net/11250/2636528 | |
dc.description.abstract | A γ-ray excess at high Galactic latitudes starting at energies 300 GeV was recently discovered in the data of the Fermi telescope. The multi-TeV γ-ray emission found has spectral characteristics at both low and high Galactic latitudes compatible with those of the IceCube neutrinos in the same sky regions. This suggests that these γ-rays are the counterpart of the IceCube neutrino signal, implying that a sizeable part of the IceCube neutrino flux originates from the Milky Way. The diffuse neutrino and γ-ray signal at high Galactic latitudes may originate either from a nearby cosmic ray "PeVatron" cosmic ray source, an extended Galactic cosmic ray halo or from decays of heavy dark matter particles. | nb_NO |
dc.language.iso | eng | nb_NO |
dc.publisher | Institute of Physics, IOP Science | nb_NO |
dc.rights | Navngivelse 4.0 Internasjonal | * |
dc.rights.uri | http://creativecommons.org/licenses/by/4.0/deed.no | * |
dc.title | Gamma-ray counterpart of the IceCube neutrinos | nb_NO |
dc.type | Journal article | nb_NO |
dc.type | Peer reviewed | nb_NO |
dc.description.version | publishedVersion | nb_NO |
dc.source.pagenumber | 1-6 | nb_NO |
dc.source.volume | 1181 | nb_NO |
dc.source.journal | Journal of Physics: Conference Series | nb_NO |
dc.source.issue | 1 | nb_NO |
dc.identifier.doi | 10.1088/1742-6596/1181/1/012052 | |
dc.identifier.cristin | 1715610 | |
dc.description.localcode | Content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. | nb_NO |
cristin.unitcode | 194,66,20,0 | |
cristin.unitname | Institutt for fysikk | |
cristin.ispublished | true | |
cristin.fulltext | original | |
cristin.qualitycode | 1 | |