First Observation of PeV-Energy Neutrinos with IceCube

Aartsen, M. G.; Abbasi, Rasha; Abdou, Y.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Altmann, D.; Auffenberg, J.; Bai, X.; Baker, M. D.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Bechet, S.; Tjus, J. Becker; Becker, Karl‐Heinz; Bell, Michael; Benabderrahmane, M. L.; BenZvi, S.; Berdermann, Jens; Berghaus, P.; Berley, D.; Bernardini, E.; Bernhard, A.; Bertrand, Daniel; Besson, D.; Binder, G.; Bindig, D.; Bissok, M.; Blaufuss, E.; Blumenthal, J.; Boersma, D. J.; Bohaichuk, S.; Böhm, C.; Bose, D.; Böser, S.; Botner, O.; Brayeur, L.; Bretz, H.-P.; Brown, A. M.; Bruijn, R.; Brünner, J.; Carson, M.; Casey, J.; Casier, M.; Chirkin, D.; Christov, A.; Christy, B.; Clark, K.; Clevermann, F.; Coenders, S.; Cohen, S.; Cowen, D. F.; Silva, A. H. Cruz; Danninger, M.; Daughhetee, J.; Davis, J.; Clercq, C. De; Ridder, S. De; Desiati, P.; With, M. de; DeYoung, Tyce; Díaz-Vélez, J. C.; Dunkman, M.; Eagan, R.; Eberhardt, B.; Eisch, J.; Ellsworth, R. W.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Fedynitch, Anatoli; Feintzeig, J.; Feusels, T.; Filimonov, K.; Finley, C.; Fischer-Wasels, T.; Flis, S.; Franckowiak, A.; Franke, Robert; Frantzen, K.; Fuchs, T.; Gaisser, T. K.; Gallagher, J.; Gerhardt, L.; Gladstone, L.; Glüsenkamp, T.; Goldschmidt, A.; Golup, G.; González, J. G.; Goodman, J. A.; Góra, Dariusz; Grant, D.; Groß, A.; Gurtner, M.; Ha, C.; Ismail, A. Haj; Hallen, P.; Hallgren, A.; Halzen, F.; Hanson, K.; Heereman, D.; Heinen, D.; Helbing, K.; Hellauer, R.; Hickford, S.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Homeier, A.; Hoshina, K.; Huelsnitz, W.; Hulth, P. O.; Hultqvist, K.; Hussain, Safeer; Ishihara, A.; Jacobi, E.; Jacobsen, J.; Jagielski, K.; Japaridze, G. S.; Jero, K.; Jlelati, O.; Kaminsky, B.; Kappes, A.; Karg, T.; Karle, A.; Kelley, J. L.; Kiryluk, J.; Kislat, Fabian; Kläs, J.; Klein, S. R.; Köhne, J. H.; Kohnen, G.; Kolanoski, H.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Krasberg, M.; Krings, K.; Kroll, G.; Kunnen, J.; Kurahashi, N.; Kuwabara, T.; Labare, M.; Landsman, H.; Larson, M. J.; Lesiak-Bzdak, M.; Leuermann, M.; Leute, J.; Lünemann, J.; Madsen, J.; Maruyama, R.; Mase, K.; Matis, H. S.; McNally, F.; Meagher, K.; Merck, M.; Mészáros, P.; Meures, T.; Miarecki, S.; Middell, E.; Milke, N.; Miller, J.; Mohrmann, L.; Montaruli, T.; Morse, R.; Nahnhauer, R.; Naumann, Uwe; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Obertacke, A.; Odrowski, S.; Olivas, A.; Olivo, M.; O’Murchadha, A.; Paul, Larissa; Pepper, J. A.; Heros, C. Pérez de los; Pfendner, C.; Pieloth, D.; Pinat, E.; Pirk, Norbert; Posselt, J.; Price, P. B.; Przybylski, G. T.; Rädel, L.; Rameez, M.; Rawlins, K.; Redl, P.; Reimann, R.; Resconi, E.; Rhode, W.; Ribordy, M.; Richman, M.; Riedel, Benedikt; Rodrigues, J. P.; Rott, C.; Ruhe, T.; Ruzybayev, B.; Ryckbosch, D.; Saba, S. M.; Salameh, T.; Sander, H. G.; Santander, M.; Sarkar, S.; Schatto, K.; Scheel, Mark A.; Scheriau, F.; Schmidt, T.; Schmitz, M.; Schoenen, S.; Schöneberg, S.; Schönwald, A.; Schukraft, A.; Schulte, L.; Schulz, O.; Seckel, D.; Sestayo, Y.; Seunarine, S.; Sheremata, C.; Smith, M. W. E.; Soiron, M.; Soldin, D.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.; Stasik, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Strahler, E. A.; Strom, Lars Rickard; Sullivan, G. W.; Taavola, H.; Taboada, I.; Tamburro, A.; Ter–Antonyan, S.; Tešić, G.; Tilav, S.; Toale, P. A.; Toscano, S.; Usner, M.; Drift, D. van der; Eijndhoven, N. van; Overloop, A. Van; Santen, J. V.; Vehring, M.; Vöge, M.; Vraeghe, M.; Walck, C.; Waldenmaier, T.; Wallraff, M.; Wasserman, R.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.; Wiebe, K.; Wiebusch, C. H.; Williams, D. R.; Wissing, H.; Wolf, M.; Wood, T. R.; Woschnagg, K.; Xu, C.; Xu, D. L.; Xu, X. W.; Yañez, J. P.; Yodh, G.; Yoshida, Shigeru; Zarzhitsky, P.; Ziemann, J.; Zierke, S.; Zilles, Anne; Zoll, M.

doi:10.1103/physrevlett.111.021103

Cited by 736 publications

(538 citation statements)

References 26 publications

(39 reference statements)

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“…IceCube collaboration has observed the neutrinos of very high energy going to beyond 2.6 PeV [1][2][3][4]. The IceCube data in the energy range 60 TeV to ∼ 3 PeV is consistent with E −2 ν neutrino spectrum following E 2 ν dN ν /dE ν 1.2 × 10 −8 GeVcm −2 s −1 sr −1 [2,3].…”

Section: Introductionsupporting

confidence: 49%

Lorentz invariance violation and IceCube neutrino events

Tomar

Mohanty

Pakvasa

2015

J. High Energ. Phys.

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The IceCube neutrino spectrum shows a flux which falls of as E −2 for sub PeV energies but there are no neutrino events observed above ∼ 3 PeV. In particular the Glashow resonance expected at 6.3 PeV is not seen. We examine a Planck scale Lorentz violation as a mechanism for explaining the cutoff of observed neutrino energies around a few PeV. By choosing the one free parameter the cutoff in neutrino energy can be chosen to be between 2 and 6.3 PeV. We assume that neutrinos (antineutrinos) have a dispersion relation E 2 = p 2 − (ξ 3 /M Pl ) p 3 , and find that both π + and π − decays are suppressed at neutrino energies of order of few PeV. We find that the µ − decay being a two-neutrino process is enhanced, whereas µ + decay is suppressed. The K + → π 0 e + ν e is also suppressed with a cutoff neutrino energy of same order of magnitude, whereas K − → π 0 e −ν e is enhanced. The n → p + e −ν e decay is suppressed (while then → p − e + ν e is enhanced). This means that theν e expected from n decay arising from p + γ → ∆ → π + n reaction will not be seen. This can explain the lack of Glashow resonance events at IceCube. If no Glashow resonance events are seen in the future then the Lorentz violation can be a viable explanation for the IceCube observations at PeV energies.

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Section: Introductionsupporting

confidence: 49%

Lorentz invariance violation and IceCube neutrino events

Tomar

Mohanty

Pakvasa

2015

J. High Energ. Phys.

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“…Supernovae interacting with fast winds of massive star clusters are plausible sources of ∼ 40 PeV protons and PeV regime gamma-ray emission and neutrinos, produced by the CRs in p-p collisions with shock-compressed ambient medium. This can possibly explain some of the neutrino events detected recently by the Ice Cube Observatory (Aartsen et al 2013, IceCube Collaboration et al 2013a, Aartsen et al 2014 which are clumped within three median angular errors from the direction to Westerlund I and the surrounding clouds associated with the TeV source detected by H.E.S.S. 1 .…”

Section: Neutrinos and Gamma-rays From Compact Clustersmentioning

confidence: 96%

Nonthermal particles and photons in starburst regions and superbubbles

Bykov

2014

Astron Astrophys Rev

114

102

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Starforming factories in galaxies produce compact clusters and loose associations of young massive stars. Fast radiation-driven winds and supernovae input their huge kinetic power into the interstellar medium in the form of highly supersonic and superalfvenic outflows. Apart from gas heating, collisionless relaxation of fast plasma outflows results in fluctuating magnetic fields and energetic particles. The energetic particles comprise a long-lived component which may contain a sizeable fraction of the kinetic energy released by the winds and supernova ejecta and thus modify the magnetohydrodynamic flows in the systems. We present a concise review of observational data and models of nonthermal emission from starburst galaxies, superbubbles, and compact clusters of massive stars. Efficient mechanisms of particle acceleration and amplification of fluctuating magnetic fields with a wide dynamical range in starburst regions are discussed. Sources of cosmic rays, neutrinos and multi-wavelength nonthermal emission associated with starburst regions including potential galactic "PeVatrons" are reviewed in the global galactic ecology context.

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“…A further impetus in searching for DM signals at these masses comes from the detection of an astrophysical high-energy neutrino flux at IceCube [13][14][15][16]. At present no point sources have been detected in the data [17][18][19] and whilst a number of purely astrophysical explanations of the flux remain, see e.g.…”

Section: Jcap02(2018)049mentioning

confidence: 99%

A search for dark matter in the Galactic halo with HAWC

Abeysekara

Albert

Alfaro

et al. 2018

J. Cosmol. Astropart. Phys.

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Abstract. The High Altitude Water Cherenkov (HAWC) gamma-ray observatory is a wide field-of-view observatory sensitive to 500 GeV -100 TeV gamma rays and cosmic rays. With its observations over 2/3 of the sky every day, the HAWC observatory is sensitive to a wide variety of astrophysical sources, including possible gamma rays from dark matter. Dark matter annihilation and decay in the Milky Way Galaxy should produce gamma-ray signals across many degrees on the sky. The HAWC instantaneous field-of-view of 2 sr enables observations of extended regions on the sky, such as those from dark matter in the Galactic halo. Here we show limits on the dark matter annihilation cross-section and decay lifetime from HAWC observations of the Galactic halo with 15 months of data. These are some of the most robust limits on TeV and PeV dark matter, largely insensitive to the dark matter morphology. These limits begin to constrain models in which PeV IceCube neutrinos are explained by dark matter which primarily decays into hadrons.

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First Observation of PeV-Energy Neutrinos with IceCube

Cited by 736 publications

References 26 publications

Lorentz invariance violation and IceCube neutrino events

Lorentz invariance violation and IceCube neutrino events

Nonthermal particles and photons in starburst regions and superbubbles

A search for dark matter in the Galactic halo with HAWC

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