Follow-up of Astrophysical Transients in Real Time with the IceCube Neutrino Observatory

Abbasi, Rasha; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Alispach, Cyril Martin; Alves, A. A.; Amin, Najia Moureen Binte; An, R.; Andeen, K.; Anderson, W. G.; Ansseau, I.; Anton, G.; Argüelles, C.; Axani, Spencer; Bai, X.; Barbano, Anastasia Maria; Barwick, S. W.; Bastian, Benjamin; Basu, Vedant; Baum, V.; Baur, S.; Bay, R.; Beatty, J. J.; Becker, K.-H.; Tjus, Julia Becker; Bellenghi, Chiara; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, Summer; Böser, S.; Botner, O.; Böttcher, Jakob; Bourbeau, Etienne; Bourbeau, J.; Bradascio, Federica; Braun, J.; Bron, S.; Brostean-Kaiser, Jannes; Burgman, A.; Busse, Raffaela; Campana, Michael; Chen, C.; Chirkin, D.; Choi, S.; Clark, Brian; Clark, K.; Classen, L.; Coleman, Alan; Collin, Gabriel; Conrad, J. M.; Coppin, Paul; Correa, Pablo; Cowen, D. F.; Cross, R.; Dave, Pranav; Clercq, C. De; DeLaunay, James; Dembinski, H.-P.; Deoskar, Kunal; Ridder, S. De; Desai, Abhishek; Desiati, P.; Vries, Krijn de; Wasseige, Gwenhaël de; DeYoung, Tyce; Dharani, Sukeerthi; Dı́az, A.; Díaz-Vélez, J. C.; Dujmović, Hrvoje; Dunkman, M.; DuVernois, Michael; Dvorak, Emily; Ehrhardt, Thomas; Eller, P.; Engel, R.; Evans, John; Evenson, P. A.; Fahey, S.; Fazely, A. R.; Fiedlschuster, Sebastian; Fienberg, Aaron; Filimonov, K.; Finley, C.; Fischer, Leander; Fox, D. B.; Franckowiak, A.; Friedman, E.; Fritz, A.; Fürst, Philipp; Gaisser, T. K.; Gallagher, John S.; Ganster, Erik; Garrappa, S.; Gerhardt, L.; Ghadimi, Ava; Gläser, Christian; Glauch, Theo; Glüsenkamp, T.; Goldschmidt, A.; González, J. G.; Goswami, Sreetama; Grant, D.; Grégoire, T.; Griffith, Z.; Griswold, Spencer; Gündüz, Mehmet; Haack, Christian; Hallgren, A.; Halliday, R.; Halve, L.; Halzen, F.; Minh, Martin Ha; Hanson, K.; Hardin, John; Harnisch, Alexander; Haungs, A.; Hauser, Simon; Hebecker, D.; Helbing, K.; Henningsen, Felix; Hettinger, Emma C.; Hickford, S.; Hignight, J.; Hill, Colton; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Hoinka, Tobias; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, M. E.; Huber, Thomas; Hultqvist, K.; Hünnefeld, Mirco; Hussain, Raamis; In, S.; Iovine, N.; Ishihara, A.; Jansson, Matti; Japaridze, G. S.; Jeong, Minjin; Jones, B. J. P.; Joppe, R.; Kang, D.; Kang, Woosik; Kang, X.; Kappes, A.; Kappesser, David; Karg, T.; Karl, Martina; Karle, A.; Katz, U.; Kauer, M.; Kellermann, Moritz; Kelley, J. L.; Kheirandish, Ali; Kim, J.; Kin, Ken'ichi; Kintscher, T.; Kiryluk, J.; Klein, S. R.; Koirala, R.; Kolanoski, H.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. 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doi:10.3847/1538-4357/abe123

Cited by 25 publications

(20 citation statements)

References 79 publications

(88 reference statements)

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“…The growing number of cosmic neutrino alerts has triggered follow-up searches for coincident detection of electromagnetic radiation, see, e.g., Abbasi et al (2021c), Garrappa et al (2019), Acciari et al (2021). On 2019 October 1, the IceCube Collaboration reported the detection of a muon track neutrino of likely astrophysical origin, IC191001A.…”

Section: Introductionmentioning

confidence: 99%

Is the High-energy Neutrino Event IceCube-200530A Associated with a Hydrogen-rich Superluminous Supernova?

Pitik

Tamborra

Angus

et al. 2022

ApJ

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The Zwicky Transient Facility follow-up campaign of alerts released by the IceCube Neutrino Observatory has led to the likely identification of the transient AT2019fdr as the source of the neutrino event IC200530A. AT2019fdr was initially suggested to be a tidal disruption event in a Narrow-Line Seyfert 1 galaxy. However, the combination of its spectral properties, color evolution, and feature-rich light curve suggests that AT2019fdr may be a Type IIn superluminous supernova. In the latter scenario, IC200530A may have been produced via inelastic proton-proton collisions between the relativistic protons accelerated at the forward shock and the cold protons of the circumstellar medium. Here, we investigate this possibility and find that at most 4.6 × 10−2 muon neutrino and antineutrino events are expected to be detected by the IceCube Neutrino Observatory within 394 days of discovery in the case of excellent discrimination of the atmospheric background. After correcting for the Eddington bias, which occurs when a single cosmic neutrino event is adopted to infer the neutrino emission at the source, we conclude that IC200530A may originate from the hydrogen-rich superluminous supernova AT2019fdr.

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Section: Introductionmentioning

confidence: 99%

Is the High-energy Neutrino Event IceCube-200530A Associated with a Hydrogen-rich Superluminous Supernova?

Pitik

Tamborra

Angus

et al. 2022

ApJ

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“…Since 2016, the IceCube multimessenger program has grown from issuing Galactic supernova alerts [ 48 ] and common data analyses matching neutrinos with early LIGO/Virgo gravitational wave candidates to a steadily expanding set of automatic filters that selects in real time rare, very high energy neutrino events that are likely to be cosmic in origin. [ 49 ] Within less than a minute of stopping in the instrumented Antarctic ice, the arrival directions of the neutrinos are reconstructed and automatically sent to the Gamma‐ray Coordinate Network for potential follow‐up by astronomical telescopes.…”

Section: Identifying Neutrino Sources: the Supermassive Black Hole Txs 0506+056mentioning

confidence: 99%

High‐Energy Neutrinos from the Cosmos

Halzen

2021

Annalen der Physik

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The IceCube project transformed a cubic kilometer of transparent natural Antarctic ice into a Cherenkov detector. It discovered PeV‐energy neutrinos originating beyond our galaxy with an energy flux that is comparable to that of GeV‐energy gamma rays and EeV‐energy cosmic rays. These neutrinos provide the only unobstructed view of the cosmic accelerators that power the highest energy radiation reaching us from the universe. The results from IceCube's first decade of operations, foremost the measurement of the diffuse neutrino flux from the universe using multiple techniques is reviewed. The multimessenger data that identified the supermassive black hole TXS 0506+056 as a source of cosmic neutrinos is subsequently reviewed and attention is drawn to accumulating indications that cosmic neutrinos are associated with gamma‐ray‐obscured active galaxies, that is, the energy in gamma rays that accompanies cosmic neutrinos emerges at MeV energies, or below. Reaching beyond 10 PeV energy, cosmic neutrinos provide a natural beam to study neutrinos themselves.

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“…It is predicted that astrophysical neutrinos are produced in the highest energy extragalactic sources such as the super-massive black holes at the centre of active galactic nuclei [46,47], the collapse of massive stars in gamma ray bursts [48,49], or in star burst galaxies [50]. Although some potential points sources have been identified and there is growing evidence for the blazar connection [51,52], the exact nature of astrophysical neutrino sources remain uncertain [53][54][55][56][57][58][59][60][61][62].…”

Section: Neutrino Sourcesmentioning

confidence: 99%

Dark matter neutrino scattering in the galactic centre with IceCube

McMullen¹,

Vincent²,

Argüelles³

et al. 2021

J. Inst.

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While there is evidence for the existence of dark matter, its properties have yet to be discovered. Simultaneously, the nature of high-energy astrophysical neutrinos detected by IceCube remains unresolved. If dark matter and neutrinos are coupled to each other, they could exhibit a non-zero elastic scattering cross section. Such an interaction between an isotropic extragalactic neutrino flux and dark matter would be concentrated in the Galactic Centre, where the dark matter column density is the greatest. This scattering would attenuate the flux of high-energy neutrinos, which could be observed in the IceCube South Pole Neutrino Observatory. In this thesis, an unbinned likelihood analysis is performed to set sensitivities for the seven year medium energy starting event cascades dataset for a signal considering possible dark matterneutrino interaction scenarios. This signal would be observed as a suppression of the high-energy astrophysical neutrino flux in the direction of the Galactic Centre. It is shown that IceCube can set constraints on possible dark matter-neutrino interactions that are complementary to constraints set by large scale structure surveys and the cosmic microwave background. i I would like to thank my supervisor Aaron Vincent at Queen's and co-supervisor Carlos Argüelles at Harvard for their support and guidance during the course of this thesis. I have been extremely lucky to have great supervisors who patiently answer all my questions and provide invaluable advice. I would also like to thank Austin Schneider for his excellent insight with this analysis. I would like to acknowledge the support of NSERC, the IceCube collaboration, the Frontenac Cluster, and the Canadian Armed Forces in making this thesis possible. I would also like to thank all my family and friends for their support during this degree. I would especially like to thank Eric and Mikayla McMullen for editing this thesis and Simran Nerval for providing feedback for my thesis presentation. I would also like to thank the members of my thesis committee, Joe Bramante and Nahee Park for their comments and discussion during the thesis defence.

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Follow-up of Astrophysical Transients in Real Time with the IceCube Neutrino Observatory

Cited by 25 publications

References 79 publications

Is the High-energy Neutrino Event IceCube-200530A Associated with a Hydrogen-rich Superluminous Supernova?

Is the High-energy Neutrino Event IceCube-200530A Associated with a Hydrogen-rich Superluminous Supernova?

High‐Energy Neutrinos from the Cosmos

Dark matter neutrino scattering in the galactic centre with IceCube

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