Establishing accretion flares from supermassive black holes as a source of high-energy neutrinos
Sjoert van Velzen, Robert Stein, M. Gilfanov, M. Kowalski, Kimitake Hayasaki, Simeon Reusch, Yuhan Yao, S. Garrappa, A. Franckowiak, Suvi Gezari, J. Nordin, C. Fremling, Y. Sharma, Lin Yan, Erik C. Kool, Daniel Stern, Patrik Milán Veres, J. Sollerman, П. С. Медведев, R. A. Sunyaev, Eric C. Bellm, Richard Dekany, Dimitri A Duev, M. J. Graham, M. M. Kasliwal, S. R. Kulkarni, Russ R. Laher, Reed Riddle, B. Rusholme
Abstract
ABSTRACT The 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.