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Constraints on Minute-Scale Transient Astrophysical Neutrino Sources
Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch, New Zealand.
DESY, D-15738 Zeuthen, Germany.
Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch, New Zealand.
Univ Libre Bruxelles, Sci Fac, CP230, B-1050 Brussels, Belgium.
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2019 (English)In: Physical Review Letters, ISSN 0031-9007, E-ISSN 1079-7114, Vol. 122, no 5, article id 051102Article in journal (Refereed) Published
Abstract [en]

High-energy neutrino emission has been predicted for several short-lived astrophysical transients including gamma-ray bursts (GRBs), core-collapse supernovae with choked jets, and neutron star mergers. IceCube's optical and x-ray follow-up program searches for such transient sources by looking for two or more muon neutrino candidates in directional coincidence and arriving within 100 s. The measured rate of neutrino alerts is consistent with the expected rate of chance coincidences of atmospheric background events and no likely electromagnetic counterparts have been identified in Swift follow-up observations. Here, we calculate generic bounds on the neutrino flux of short-lived transient sources. Assuming an E-2.5 neutrino spectrum, we find that the neutrino flux of rare sources, like long gamma-ray bursts, is constrained to < 5% of the detected astrophysical flux and the energy released in neutrinos (100 GeV to 10 PeV) by a median bright GRB-like source is < 10(52.5) erg. For a harder E-2.13 neutrino spectrum up to 30% of the flux could be produced by GRBs and the allowed median source energy is < 10(52) erg. A hypothetical population of transient sources has to be more common than 10(-5) Mpc(-3) yr(-1) (5 x 10(-8) Mpc(-3) yr(-1) for the E-2.13 spectrum) to account for the complete astrophysical neutrino flux.

Place, publisher, year, edition, pages
AMER PHYSICAL SOC , 2019. Vol. 122, no 5, article id 051102
National Category
Subatomic Physics Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-378535DOI: 10.1103/PhysRevLett.122.051102ISI: 000458147300005OAI: oai:DiVA.org:uu-378535DiVA, id: diva2:1298440
Funder
German Research Foundation (DFG)Swedish Research CouncilSwedish National Infrastructure for Computing (SNIC)Knut and Alice Wallenberg FoundationAustralian Research CouncilAvailable from: 2019-03-22 Created: 2019-03-22 Last updated: 2019-05-21Bibliographically approved

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Botner, OlgaBurgman, AlexanderHallgren, AllanPérez de los Heros, CarlosUnger, Elisabeth

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