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Fermi/LAT counterparts of IceCube neutrinos above 100 TeV
Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC). Indian Institute of Technology Kharagpur, India; Universität Erlangen-Nürnberg, Germany.
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Number of Authors: 102018 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 620, article id A174Article in journal (Refereed) Published
Abstract [en]

The IceCube Collaboration has published four years of data and the observed neutrino flux is significantly in excess of the expected atmospheric background. Due to the steeply falling atmospheric background spectrum, events at the highest energies are most likely extraterrestrial. In our previous approach we have studied blazars as the possible origin of the High-Energy Starting Events (HESE) neutrino events at PeV energies. In this work we extend our study to include all HESE neutrinos (which does not include IC 170922A) at or above a reconstructed energy of 100 TeV, but below 1 PeV. We study the X-ray and gamma-ray data of all (similar to 200) 3LAC blazars that are positionally consistent with the neutrino events above 100 TeV to determine the maximum neutrino flux from these sources. This larger sample allows us to better constrain the scaling factor between the observed and maximum number of neutrino events. We find that when we consider a realistic neutrino spectrum and other factors, the number of neutrinos is in good agreement with the detected number of IceCube HESE events. We also show that there is no direct correlation between Fermi/LAT gamma-ray flux and the IceCube neutrino flux and that the expected number of neutrinos is consistent with the non-detection of individual bright blazars.

Place, publisher, year, edition, pages
2018. Vol. 620, article id A174
Keywords [en]
neutrinos, galaxies: active, quasars: general, BL Lacertae objects: general
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-163679DOI: 10.1051/0004-6361/201834183ISI: 000453301200006OAI: oai:DiVA.org:su-163679DiVA, id: diva2:1280336
Available from: 2019-01-18 Created: 2019-01-18 Last updated: 2019-01-18Bibliographically approved

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