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000619704 0247_ $$2arXiv$$aarXiv:2111.09391
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000619704 088__ $$2arXiv$$aarXiv:2111.09391
000619704 082__ $$a520
000619704 1001_ $$0P:(DE-HGF)0$$avan Velzen, Sjoert$$b0$$eCorresponding author
000619704 245__ $$aEstablishing accretion flares from supermassive black holes as a source of high-energy neutrinos
000619704 260__ $$c2024
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000619704 500__ $$aMonthly Notices of the Royal Astronomical Society (2024), Volume 529, Issue 3, 2559-2576. Accepted for publication in MNRAS  AF received funding from the German Science Foundation DFG,within the Collaborative Research Center SFB1491 ‘Cosmic Inter-acting Matters – From Source to Signal’.
000619704 520__ $$aThe origin of cosmic high-energy neutrinos remains largely unexplained. For high-energy neutrino alerts from IceCube, a coincidence with time-variable emission has been seen for three different types of accreting black holes: (1) a gamma-ray flare from a blazar (TXS 0506+056), (2) an optical transient following a stellar tidal disruption event (TDE; AT2019dsg), and (3) an optical outburst from an active galactic nucleus (AGN; AT2019fdr). For the latter two sources, infrared follow-up observations revealed a powerful reverberation signal due to dust heated by the flare. This discovery motivates a systematic study of neutrino emission from all supermassive black hole with similar dust echoes. Because dust reprocessing is agnostic to the origin of the outburst, our work unifies TDEs and high-amplitude flares from AGN into a population that we dub accretion flares. Besides the two known events, we uncover a third flare that is coincident with a PeV-scale neutrino (AT2019aalc). Based solely on the optical and infrared properties, we estimate a significance of 3.6σ for this association of high-energy neutrinos with three accretion flares. Our results imply that at least ∼10 per cent of the IceCube high-energy neutrino alerts could be due to accretion flares. This is surprising because the sum of the fluence of these flares is at least three orders of magnitude lower compared to the total fluence of normal AGN. It thus appears that the efficiency of high-energy neutrino production in accretion flares is increased compared to non-flaring AGN. We speculate that this can be explained by the high Eddington ratio of the flares.
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000619704 536__ $$0G:(DE-HGF)2018_VH-NG-1202$$aVH-NG-1202 - Identifying the Sources of High-Energy Neutrinos with Multi-Messenger Observations (2018_VH-NG-1202)$$c2018_VH-NG-1202$$x1
000619704 536__ $$0G:(GEPRIS)445052434$$aDFG project G:(GEPRIS)445052434 - SFB 1491: Das Wechselspiel der kosmischen Materie - von der Quelle bis zum Signal (445052434)$$c445052434$$x2
000619704 588__ $$aDataset connected to CrossRef, INSPIRE, Journals: bib-pubdb1.desy.de
000619704 650_7 $$2INSPIRE$$ablack hole: accretion
000619704 650_7 $$2INSPIRE$$aacceleration: efficiency
000619704 650_7 $$2INSPIRE$$aparticle: acceleration
000619704 650_7 $$2INSPIRE$$aoptical
000619704 650_7 $$2INSPIRE$$aAGN
000619704 650_7 $$2INSPIRE$$atime dependence
000619704 650_7 $$2INSPIRE$$aneutrino: energy: high
000619704 650_7 $$2INSPIRE$$ablazar
000619704 650_7 $$2INSPIRE$$ainfrared
000619704 650_7 $$2INSPIRE$$agamma ray
000619704 650_7 $$2INSPIRE$$asignature
000619704 650_7 $$2autogen$$aneutrinos
000619704 650_7 $$2autogen$$agalaxies: active
000619704 650_7 $$2autogen$$atransients: tidal disruption events
000619704 693__ $$0EXP:(DE-H253)IceCube-20150101$$5EXP:(DE-H253)IceCube-20150101$$eIceCube South Pole Neutrino Observatory$$x0
000619704 7001_ $$aStein, Robert$$b1
000619704 7001_ $$aGilfanov, Marat$$b2
000619704 7001_ $$0P:(DE-H253)PIP1006050$$aKowalski, Marek$$b3$$udesy
000619704 7001_ $$aHayasaki, Kimitake$$b4
000619704 7001_ $$aReusch, Simeon$$b5
000619704 7001_ $$aYao, Yuhan$$b6
000619704 7001_ $$0P:(DE-H253)PIP1022301$$aGarrappa, Simone$$b7$$udesy
000619704 7001_ $$0P:(DE-H253)PIP1006092$$aFranckowiak, Anna$$b8
000619704 7001_ $$aGezari, Suvi$$b9
000619704 7001_ $$0P:(DE-H253)PIP1032718$$aNordin, Jakob$$b10
000619704 7001_ $$aFremling, Christoffer$$b11
000619704 7001_ $$aSharma, Yashvi$$b12
000619704 7001_ $$aYan, Lin$$b13
000619704 7001_ $$aKool, Erik C.$$b14
000619704 7001_ $$aStern, Daniel$$b15
000619704 7001_ $$aVeres, Patrik M.$$b16
000619704 7001_ $$aSollerman, Jesper$$b17
000619704 7001_ $$aMedvedev, Pavel$$b18
000619704 7001_ $$aSunyaev, Rashid$$b19
000619704 7001_ $$aBellm, Eric C.$$b20
000619704 7001_ $$aDekany, Richard G.$$b21
000619704 7001_ $$aDuev, Dimitri A.$$b22
000619704 7001_ $$aGraham, Matthew J.$$b23
000619704 7001_ $$aKasliwal, Mansi M.$$b24
000619704 7001_ $$aKulkarni, Shrinivas R.$$b25
000619704 7001_ $$aLaher, Russ R.$$b26
000619704 7001_ $$aRiddle, Reed L.$$b27
000619704 7001_ $$aRusholme, Ben$$b28
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000619704 9131_ $$0G:(DE-HGF)POF4-613$$1G:(DE-HGF)POF4-610$$2G:(DE-HGF)POF4-600$$3G:(DE-HGF)POF4$$4G:(DE-HGF)POF$$aDE-HGF$$bForschungsbereich Materie$$lMatter and the Universe$$vMatter and Radiation from the Universe$$x0
000619704 9141_ $$y2024
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