Erratum: Constraints on the extremely-high energy cosmic neutrino flux with the IceCube 2008-2009 data [Phys. Rev. D<b>83</b>, 092003 (2011)]

Abbasi, Rasha; Abdou, Y.; Abu‐Zayyad, T.; Adams, J. S.; Aguilar, J. A.; Ahlers, M.; Andeen, K.; Auffenberg, J.; Bai, X.; Baker, M. D.; Barwick, S. W.; Bay, R.; Alba, J. L. Bazo; Beattie, K.; Beatty, J. J.; Bechet, S.; Becker, J.; Becker, K.-H.; Benabderrahmane, M. L.; BenZvi, S.; Berdermann, Jens; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand, Daniel; Besson, D.; Bindig, D.; Bissok, M.; Blaufuss, E.; Blumenthal, J.; Boersma, D. J.; Böhm, Christoph; Bose, D.; Böser, S.; Botner, O.; Braun, J.; Brown, A. M.; Buitink, S.; Carson, M.; Chirkin, D.; Christy, B.; Clem, J.; Clevermann, F.; Cohen, S.; Colnard, C.; Cowen, D. F.; D’Agostino, M. V.; Danninger, M.; Daughhetee, J.; Davis, J.; Clercq, C. De; Demirörs, L.; Denger, T.; Depaepe, O.; Descamps, F.; Desiati, P.; Vries-Uiterweerd, G. de; DeYoung, T.; Díaz-Vélez, J. C.; Dierckxsens, M.; Dreyer, J.; Dumm, J. P.; Ehrlich, R.; Eisch, J.; Ellsworth, R. W.; Engdegård, O.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Fedynitch, Anatoli; Feusels, T.; Filimonov, K.; Finley, C.; Fischer-Wasels, T.; Foerster, M. M.; Fox, B. D.; Franckowiak, A.; Franke, Robert; Gaisser, T. K.; Gallagher, J.; Geisler, M.; Gerhardt, L.; Gladstone, L.; Glüsenkamp, T.; Goldschmidt, A.; Goodman, J. A.; Góra, D.; Grant, D.; Griesel, T.; Groß, A.; Grullon, S.; Gurtner, M.; Ha, C.; Hallgren, A.; Halzen, F.; Han, K.; Hanson, K.; Heinen, D.; Helbing, K.; Herquet, P.; Hickford, S.; Hill, G. C.; Hoffman, K. D.; Homeier, A.; Hoshina, K.; Hubert, D.; Huelsnitz, W.; Hülß, J.-P.; Hulth, P. O.; Hultqvist, K.; Hussain, Shahid; Ishihara, A.; Jacobsen, J.; Japaridze, G. S.; Johansson, H.; Joseph, J.; Kampert, K.‐H.; Kappes, A.; Karg, T.; Karle, A.; Kelley, J. L.; Kenny, Patrick; Kiryluk, J.; Kislat, Fabian; Klein, S. R.; Köhne, J. H.; Kohnen, G.; Kolanoski, H.; Köpke, L.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Kowarik, T.; Krasberg, M.; Krings, T.; Kroll, G.; Kuwabara, T.; Labare, M.; Lafèbre, S.; Laihem, K.; Landsman, H.; Larson, M. J.; Lauer, R.; Lünemann, J.; Madsen, J.; Majumdar, P.; Marotta, Anna; Maruyama, R.; Mase, K.; Matis, H. S.; Meagher, K.; Merck, M.; Mészáros, P.; Meures, T.; Middell, E.; Milke, N.; Miller, J.; Montaruli, T.; Morse, R.; Movit, S. M.; Nahnhauer, R.; Nam, J. W.; Naumann, Uwe; Nießen, P.; Nygren, D. R.; Odrowski, S.; Olivas, A.; Olivo, M.; O’Murchadha, A.; Ono, M.; Panknin, S.; Paul, Larissa; Heros, C. Pérez de los; Petrović, J.; Piegsa, A.; Pieloth, D.; Porrata, R.; Posselt, J.; Price, P. B.; Przybylski, G. T.; Rawlins, K.; Redl, P.; Resconi, E.; Rhode, W.; Ribordy, M.; Rizzo, A.; Rodrigues, J. P.; Roth, Peter M.; Rothmaier, F.; Rott, C.; Ruhe, T.; Rutledge, D.; Ruzybayev, B.; Ryckbosch, D.; Sander, H.G.; Santander, M.; Sarkar, S.; Schatto, K.; Schmidt, T.; Schönwald, A.; Schukraft, A.; Schultes, A.; Schulz, O.; Schunck, M.; Seckel, D.; Semburg, B.; Seo, S. h.; Sestayo, Y.; Seunarine, S.; Silvestri, A.; Slipak, A.; Spiczak, G. M.; Spiering, Christian; Stamatikos, M.; Stanev, T.; Stephens, G.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Stoyanov, S.; Strahler, E. A.; Straszheim, T.; Stür, M.; Sullivan, G. W.; Swillens, Q.; Taavola, H.; Taboada, I.; Tamburro, A.; Tepe, A.; Ter–Antonyan, S.; Tilav, S.; Toale, P. A.; Toscano, S.; Tosi, D.; Turčan, D.; Eijndhoven, N. van; Vandenbroucke, J.; Overloop, A. Van; Santen, J. V.; Vehring, M.; Vöge, M.; Walck, C.; Waldenmaier, T.; Wallraff, M.; Walter, Michael; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.; Wiebe, K.; Wiebusch, C. H.; Williams, D. R.; Wischnewski, R.; Wissing, H.; Wolf, M.; Wood, T. R.; Woschnagg, K.; Xu, C.; Xu, Xianbo; Yodh, G.; Yoshida, Shigeru; Zarzhitsky, P.

doi:10.1103/physrevd.84.079902

Cited by 39 publications

(70 citation statements)

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“…For IceCube we adopt the exposure as a function of declination (which uniquely translates to zenith angle in the case of IceCube) and energy as it is given in Ref. [52] and normalize it to the actual IceCube exposure of Ref. [39].…”

Section: Analysis and Discussionmentioning

confidence: 99%

Hadronically decaying heavy dark matter and high-energy neutrino limits

Kuznetsov

2017

Jetp Lett.

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We consider dark matter consisting of long--living particles with masses $10^{7}~\lesssim~M~\lesssim~10^{16}$ GeV decaying through hadronic channel as a source of high energy neutrino. Using recent data on high energy neutrino from IceCube and Pierre Auger experiments we derive the upper-limits on neutrino flux from dark matter decay and constraints on dark matter parameter space. For the dark matter masses of order $10^8$ GeV the constraints derived are slightly stronger than those obtained for the same dark matter model using the high energy gamma-ray limits.Comment: 12 pages, 5 figures, minor corrections in text, results unchanged, published in JETP Letter

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Section: Analysis and Discussionmentioning

confidence: 99%

Hadronically decaying heavy dark matter and high-energy neutrino limits

Kuznetsov

2017

Jetp Lett.

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“…The energy spectrum from a cosmic signal (either point-like or diffuse) is expected to be harder than that of atmospheric neutrinos. This latter, as measured by IceCube [35,36] and ANTARES [37], depends on energy as ∝ E −3.7 . The signal should exceed the background above a certain energy threshold.…”

Section: A the Directional Cosmic Neutrino Fluxmentioning

confidence: 91%

Constraints to a Galactic component of the Ice Cube cosmic neutrino flux from ANTARES

Spurio

2014

Phys. Rev. D

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The IceCube evidence for cosmic neutrinos in the high-energy starting events (HESE) sample has inspired a large number of hypothesis on their origin, mainly due to the poor precision on the measurement of the direction of showering events. The fact that most of HESE are downward going suggests a possible Galactic component. This could be originated either by a single point-like source or to a directional excess from an extended Galactic region. These hypotheses are reviewed and constrained, using the present available upper limits from the ANTARES neutrino telescope.ANTARES detects νµ from sources in the Southern sky with an effective area larger than that providing the IceCube HESE for Eν < 60 TeV and a factor of about two smaller at 1 PeV. The use of the νµ signal enables an accurate measurement of the incoming neutrino direction. The Galactic signal allowed by the IceCube HESE and the corresponding ANTARES limits are studied in terms of a power law flux E −Γ , with spectral index Γ ranging from 2.0 to 2.5 to cover most astrophysical models.arXiv:1409.4552v2 [astro-ph.HE]

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“…The all flavor diffuse neutrino flux has been constrained at EeV energies by the unsuccessful searches by IceCube [7] and Auger [8], which imply the approximate bound E 2 ν dΦ ν /dE < 3 × 10 −7 GeV/cm 2 s sr at EeV energies. Moreover, in proton scenarios a stronger bound has been obtained indirectly from the so-called cascade decays [9].…”

Section: Neutrino Fluxes From Uhecr Protonsmentioning

confidence: 99%

“…The overall shape of the spectrum is found to be in reasonable agreement with the measured one above the ankle region. We also display the spectrum measured by the Hires Collaboration [22], and the bounds on the all flavor neutrino fluxes obtained by IceCube [7], Auger [8] and Anita [23].…”

Section: Neutrino Fluxes From Uhecr Protonsmentioning

confidence: 99%

Strong Spin–Orbit Interactions in an InAlAs/InGaAs/InAlAs Two-Dimensional Electron Gas by Weak Antilocalization Analysis

Sun

Zhou

et al. 2009

jjap

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We discuss the possibility that the PeV neutrinos recently observed by IceCube are produced by the interactions of extragalactic cosmic rays during their propagation through the radiation backgrounds. We show that the fluxes resulting from the decays of neutrons produced in the interactions of cosmic ray protons with the CMB background are suppressed (E 2 ν dΦ ν /dE < 10 −10 GeV/cm 2 s sr), with those resulting from the decays of pions produced in the interactions with the UV/optical/IR backgrounds being the dominant ones at PeV energies. The anti-neutrino fluxes produced by the decay of neutrons resulting from the photodisintegration of heavy nuclei with CMB photons are also shown to be quite suppressed (E 2 ν dΦ ν /dE < 10 −11 GeV/cm 2 s sr), while those produced by photo-pion processes with UV/optical/IR backgrounds may be larger, although they are not expected to be above those achievable in the pure proton case. Scenarios with mixed composition and low cutoff rigidities can lead to PeV neutrino fluxes enhanced with respect to those in the pure Fe scenarios. We also discuss the possible impact of the Glashow resonance for the detection of these scenarios, showing that it plays a moderate role.Keywords: ultra high energy cosmic rays, cosmological neutrinos, ultra high energy photons and neutrinos ArXiv ePrint: 1209.4033

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Erratum: Constraints on the extremely-high energy cosmic neutrino flux with the IceCube 2008-2009 data [Phys. Rev. D83, 092003 (2011)]

Cited by 39 publications

References 0 publications

Hadronically decaying heavy dark matter and high-energy neutrino limits

Hadronically decaying heavy dark matter and high-energy neutrino limits

Constraints to a Galactic component of the Ice Cube cosmic neutrino flux from ANTARES

Strong Spin–Orbit Interactions in an InAlAs/InGaAs/InAlAs Two-Dimensional Electron Gas by Weak Antilocalization Analysis

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