The candidate tidal disruption event AT2019fdr coincident with a high-energy neutrino

Reusch, Simeon; Stein, Robert; Kowalski, Marek; van Velzen, Sjoert; Franckowiak, Anna; Lunardini, Cecilia; Murase, Kohta; Winter, Walter; Miller-Jones, James C. A.; Kasliwal, Mansi M.; Gilfanov, Marat; Garrappa, Simone; Paliya, Vaidehi S.; Ahumada, Tomas; Anand, Shreya; Barbarino, Cristina; Bellm, Eric C.; Brinnel, Valery; Buson, Sara; Cenko, S. Bradley; Coughlin, Michael W.; De, Kishalay; Dekany, Richard; Frederick, Sara; Gal-Yam, Avishay; Gezari, Suvi; Giroletti, Marcello; Graham, Matthew J.; Karambelkar, Viraj; Kimura, Shigeo S.; Kong, Albert K. H.; Kool, Erik C.; Laher, Russ R.; Medvedev, Pavel; Necker, Jannis; Nordin, Jakob; Perley, Daniel A.; Rigault, Mickael; Rusholme, Ben; Schulze, Steve; Schweyer, Tassilo; Singer, Leo P.; Sollerman, Jesper; Strotjohann, Nora Linn; Sunyaev, Rashid; van Santen, Jakob; Walters, Richard; Zhang, B. Theodore; Zimmerman, Erez

doi:10.48550/arxiv.2111.09390

Cited by 11 publications

(16 citation statements)

References 126 publications

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“…After the submission of this work, we notice recent reports on more neutrino events associated with the time-variable emission from accreting SMBHs (van Velzen et al 2021a;Reusch et al 2021), among which AT2019fdr is a TDE candidate in a Narrow-Line Seyfert 1 AGN in which the BLR clouds should exist. Moreover, the neutrino events lag the optical outbursts by half one year to one year (van Velzen et al 2021a), consistent with the assumption that clouds exist at the distance of ∼ 10 −2 pc from the central BH if the outflow velocity is in the order of 10 9 cm s −1 .…”

Section: Conclusion and Discussionmentioning

confidence: 87%

Could TDE outflows produce the PeV neutrino events?

Wu,

Mou,

Wang

et al. 2021

Preprint

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The origin of ultra-high energy neutrinos still lacks observational evidence, besides, the physical mechanism is also unclear. There is an association of a PeV neutrino event (IceCube-191001A) with an optical tidal disruption event (TDE, AT2019dsg) which was detected 6 months ahead from IceCube-191001A. The numerical simulations and observations suggested that a TDE can produce ultrafast outflows, which will interact with clouds near the supermassive black hole. In this paper, we study the interactions between TDE outflows and clouds and the possible production. In the shock waves generated by the outflow-cloud interactions, protons can be accelerated to ∼ 60 PeV with the outflow velocity 0.07 c and kinetic luminosity 10 45 erg/s. PeV neutrinos can be produced through hadronic reactions. The calculation illustrates that the expected PeV neutrino event from AT2019dsg is 0.014 for a power-law proton energy distribution of Γ = 1.5 and 0.0016 for Γ = 1.9. The GeV -TeV γ-rays through hadronic processes are lower than the present observed limits. Outflows escaped from the TDE center colliding with clouds, which also can naturally explain the half-year delay between the neutrino event and TDE.

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Section: Conclusion and Discussionmentioning

confidence: 87%

Could TDE outflows produce the PeV neutrino events?

Wu,

Mou,

Wang

et al. 2021

Preprint

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“…This TDE was detected in the radio and X-ray bands, and accompanied by infrared echo emission. AT 2019fdr was another very luminous optical transient, associated with IceCube-200530A (140). The optical luminosity at the peak is LOUV ∼ 10 45 erg s −1 , and the neutrino was seen 320 days after the peak.…”

Section: Violent Transientsmentioning

confidence: 99%

High-Energy Extragalactic Neutrino Astrophysics

Kurahashi,

Murase,

Santander

2022

Preprint

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The detection of an astrophysical flux of neutrinos in the TeV-PeV energy range by the IceCube observatory has opened new possibilities for the study of extreme cosmic accelerators. The apparent isotropy of the neutrino arrival directions favors an extragalactic origin for this flux, potentially created by a large population of distant sources. Recent evidence for the detection of neutrino emission from extragalactic sources include the active galaxies TXS 0506+056 and NGC 1068. We here review the current status of the search for the sources of the high-energy neutrino flux, concentrating on its extragalactic contribution. We discuss the implications of these observations for multimessenger studies of cosmic sources and present an outlook for how additional observations by current and future instruments will help address fundamental questions in the emerging field of high-energy neutrino astronomy.

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“…4 MeV, there is also a contribution from radiogenic neutrinos originating from the decay of 40 K, 232 Th, and 238 U within the Earth. The IBD sample also includes a small number of accidental DC signals induced by the decay of radioactive impurities, additional radioactive products from cosmic-ray muon spallation [32,35], and the alpha-induced 13 C(α,n) 16 O reaction in the liquid scintillator.…”

Section: Electron Antineutrino Selection In Kamland and Background Es...mentioning

confidence: 99%

“…The diffuse astrophysical neutrino spectrum, however, appears to disfavour a single-zone model [11,12], in which the high-energy neutrinos are produced in a single emission region. The most recent studies have reported a 2.9σ neutrino excess at the coordinates of NGC 1068 [13], a radio quiet AGN; a 2.6σ excess compatible with neutrino production in the cores of AGNs [14]; and the association of two radio-emitting tidal disruption events, AT2019dsg and AT2019fdr, with a ∼0.2 PeV and ∼0.08 PeV neutrino [15,16], respectively.…”

Section: Introductionmentioning

confidence: 99%

KamLAND's search for correlated low-energy electron antineutrinos with astrophysical neutrinos from IceCube

Abe,

Asami,

Eizuka

et al. 2022

Preprint

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We report the results of a search for MeV-scale astrophysical neutrinos in KamLAND presented as an excess in the number of coincident neutrino interactions associated with the publicly available high-energy neutrino datasets from the IceCube Neutrino Observatory. We find no statistically significant excess in the number of observed low-energy electron antineutrinos in KamLAND, given a coincidence time window of ±500 s, ±1,000 s, ±3,600 s, and ±10,000 s around each of the IceCube neutrinos. We use this observation to present limits from 1.8 MeV to 100 MeV on the electron antineutrino fluence, assuming a mono-energetic flux. We then compare the results to several astrophysical measurements performed by IceCube and place a limit at the 90% confidence level on the electron antineutrino isotropic thermal luminosity from the TXS 0506+056 blazar.

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The candidate tidal disruption event AT2019fdr coincident with a high-energy neutrino

Cited by 11 publications

References 126 publications

Could TDE outflows produce the PeV neutrino events?

Could TDE outflows produce the PeV neutrino events?

High-Energy Extragalactic Neutrino Astrophysics

KamLAND's search for correlated low-energy electron antineutrinos with astrophysical neutrinos from IceCube

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