Determination of the atmospheric neutrino flux and searches for new physics with AMANDA-II

Abbasi, Rasha; Abdou, Y.; Ackermann, M.; Adams, J.; Ahlers, M.; Andeen, K.; Auffenberg, J.; Bai, X.; Baker, M. D.; Barwick, S. W.; Bay, R.; Alba, J. L. Bazo; Beattie, K.; Bechet, S.; Becker, J. K.; Becker, K. H.; Benabderrahmane, M. L.; Berdermann, Jens; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand, Daniel; Besson, D.; Bissok, M.; Blaufuss, E.; Boersma, D. J.; Böhm, C.; Bolmont, J.; Böser, S.; Botner, O.; Bradley, L.; Braun, J.; Breder, D.; Burgess, T.; Castermans, T.; Chirkin, D.; Christy, B.; Clem, J.; Cohen, S.; Cowen, D. F.; D’Agostino, M. V.; Danninger, M.; Day, C. T.; Clercq, C. De; Demirörs, L.; Depaepe, O.; Descamps, F.; Desiati, P.; Vries-Uiterweerd, G. de; DeYoung, T.; Díaz–Vélez, Juan Carlos; Dreyer, J.; Dumm, J. P.; Duvoort, M. R.; Edwards, W. R.; Ehrlich, R.; Eisch, J.; Ellsworth, R. W.; Engdegård, O.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Feusels, T.; Filimonov, K.; Finley, C.; Foerster, M. M.; Fox, B. D.; Franckowiak, A.; Franke, Robert; Gaisser, T. K.; Gallagher, J.; Ganugapati, R.; Gerhardt, L.; Gladstone, L.; Goldschmidt, A.; Goodman, J. A.; Gozzini, R.; Grant, D.; Griesel, T.; Groß, A.; Grullon, S.; Gunasingha, R. M.; Gurtner, M.; Ha, C.; Hallgren, A.; Halzen, F.; Han, K.; Hanson, K.; Hasegawa, Y.; Heise, J.; Helbing, K.; Herquet, P.; Hickford, S.; Hill, G. C.; Hoffman, K. D.; Hoshina, K.; Hubert, D.; Huelsnitz, W.; Hülß, J.-P.; Hulth, P. O.; Hultqvist, K.; Hussain, Shahid; Imlay, R.; Inaba, M.; 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.; Klepser, S.; Knops, S.; Kohnen, G.; Kolanoski, H.; Köpke, L.; Kowalski, M.; Kowarik, T.; Krasberg, M.; Kuêhn, K.; Kuwabara, T.; Labare, M.; Laihem, K.; Landsman, H.; Lauer, R.; Leich, H.; Lennarz, D.; Lücke, Andreas; Lundberg, J.; Lünemann, J.; Madsen, J.; Majumdar, P.; Maruyama, R.; Mase, K.; Matis, H. S.; McParland, C.; Meagher, K.; Merck, M.; Mészáros, P.; Middell, E.; Milke, N.; Miyamoto, H.; Mohr, Anna; Montaruli, T.; Morse, R.; Movit, S. M.; Münich, K.; Nahnhauer, R.; Nam, J. W.; Nießen, P.; Nygren, D. R.; Odrowski, S.; Olivas, A.; Olivo, M.; Ono, M.; Panknin, S.; Patton, S.; Heros, C. Pérez de los; Petrović, J.; Piegsa, A.; Pieloth, D.; Pohl, A. C.; Porrata, R.; Potthoff, Nils; Price, P. B.; Prikockis, M.; 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.; Roucelle, C.; Rutledge, D.; Ryckbosch, D.; Sander, H. G.; Sarkar, S.; Satalecka, K.; Schlenstedt, S.; Schmidt, T.; Schneider, D.; Schukraft, A.; Schulz, O.; Schunck, M.; Seckel, D.; Semburg, B.; Seo, S. h.; Sestayo, Y.; Seunarine, S.; Silvestri, A.; Slipak, A.; Spiczak, G. M.; Spiering, C.; Stanev, T.; Stephens, G.; Stezelberger, T.; Stokstad, R. G.; Stoufer, M. C.; Stoyanov, S.; Strahler, E. A.; Straszheim, T.; Sulanke, K.-H.; Sullivan, G. W.; Swillens, Q.; Taboada, I.; Tarasova, O.; Tepe, A.; Ter–Antonyan, S.; Terranova, C.; Tilav, S.; Tluczykont, M.; Toale, P. A.; Tosi, D.; Turčan, D.; Eijndhoven, N. van; Vandenbroucke, J.; Overloop, A. Van; Voigt, B.; Walck, C.; Waldenmaier, T.; Walter, Michael; Wendt, C.; Westerhoff, S.; Whitehorn, N.; Wiebusch, C. H.; Wiedemann, Armin; Wikström, G.; Williams, D. R.; Wischnewski, R.; Wissing, H.; Woschnagg, K.; Xu, X. W.; Yodh, G.; Yoshida, Shigeru

doi:10.1103/physrevd.79.102005

Cited by 98 publications

(71 citation statements)

References 78 publications

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“…The coloured contours show the range of oscillation-averaged flavor ratios based on the unitarity of the neutrino mixing matrix. Figure 16 shows the results of an analysis of atmospheric muon neutrino data in the range 100 GeV to 10 TeV taken by AMANDA-II in the years 2000 to 2006 [109]. The data was binned into two-dimensional histograms in terms of the number of hit optical modules (as a measure of energy) and the zenith angle (cos θ zen ).…”

Section: Effective Hamiltoniansmentioning

confidence: 99%

Probing particle physics with IceCube

2018

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The IceCube observatory located at the South Pole is a cubic-kilometre optical Cherenkov telescope primarily designed for the detection of high-energy astrophysical neutrinos. IceCube became fully operational in 2010, after a seven-year construction phase, and reached a milestone in 2013 by the first observation of cosmic neutrinos in the TeV-PeV energy range. This observation does not only mark an important breakthrough in neutrino astronomy, but it also provides a new probe of particle physics related to neutrino production, mixing, and interaction. In this review we give an overview of the various possibilities how IceCube can address fundamental questions related to the phenomena of neutrino oscillations and interactions, the origin of dark matter, and the existence of exotic relic particles, like monopoles. We will summarize recent results and highlight future avenues.Keywords IceCube · physics beyond the Standard Model · neutrino telescopes · neutrino oscillation · neutrino interactions · sterile neutrinos · dark matter · magnetic monopoles PACS 95.35.+d · 14.80.Hv · 13.15.+g · 14.60.Lm arXiv:1806.05696v1 [astro-ph.HE]

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Section: Effective Hamiltoniansmentioning

confidence: 99%

Probing particle physics with IceCube

2018

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“…We have also checked the flux of atmospheric neutrinos to be expected within 1 angular resolution; see, e.g., Ref. [40]. It turns out that, especially in the energy range between 100 GeV and 10 TeV, where Earth attenuation effects are relatively small, the IceCube-40 point source sensitivities for upgoing events are already touching the atmospheric neutrino background in the most conservative (systematics) case for the atmospheric neutrino flux.…”

Section: Methods and Impact Of The Spectral Shapementioning

confidence: 99%

Interpretation of neutrino flux limits from neutrino telescopes on the Hillas plot

Winter

2012

Phys. Rev. D

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We discuss the interplay between spectral shape and detector response beyond a simple E À2 neutrino flux at neutrino telescopes, using the example of time-integrated point source searches using IceCube-40 data. We use a self-consistent model for the neutrino production, in which protons interact with synchrotron photons from coaccelerated electrons, and we fully take into account the relevant pion and kaon production modes, the flavor composition at the source, flavor mixing, and magnetic field effects on the secondaries (pions, muon, and kaons). Since some of the model parameters can be related to the Hillas parameters R (size of the acceleration region) and B (magnetic field), we relate the detector response to the Hillas plane. In order to compare the response to different spectral shapes, we use the energy flux density as a measure for the pion production efficiency times luminosity of the source. We demonstrate that IceCube has a very good reach in this quantity for active galactic nuclei and jets for all source declinations, while the spectra of sources with strong magnetic fields are found outside the optimal reach. We also demonstrate where neutrinos from kaon decays and muon tracks from decays can be relevant for the detector response. Finally, we point out the complementarity between IceCube and other experiments sensitive to high-energy neutrinos, using the example of 2004-2008 Earth-skimming neutrino data from Auger. We illustrate that Auger, in principle, is more sensitive to the parameter region in the Hillas plane from which the highest-energetic cosmic rays may be expected in this model.

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“…Euan Richard Figure 1: The measured energy spectra of the atmospheric ν e +ν e and ν µ +ν µ fluxes at SK, shown in comparison to measurements by Frejus [19], AMANDA-II [20,21], and IceCube [22,24,23]. The HKKM11 [16] model predictions are also shown in solid (with oscillation) and dashed (without oscillation) lines.…”

Section: Measurements Of the Atmospheric Neutrino Flux At Super-kamiomentioning

confidence: 98%

“…These models are based on data such as the primary cosmic ray proton flux and the secondary muon flux, measured in the atmosphere by particle detectors on balloons and spacecraft, and hadron production measured in accelerator experiments. Direct experimental measurements of the flux energy spectra were made by the Frejus [19] collaboration (before neutrino oscillation was known), and more recently by the AMANDA-II [20,21] and IceCube [22,23,24] collaborations at higher energies (up to the 100 TeV range).…”

Section: Introductionmentioning

confidence: 99%

Measurements of the Atmospheric Neutrino Flux at Super-Kamiokande

Richard¹,

Okumura²,

Kajita³

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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Three direct measurements of the atmospheric ν e +ν e and ν µ +ν µ neutrino fluxes were performed using the Super-Kamiokande water Cherenkov detector: the directionally-integrated energy spectra, the azimuthal spectra, and the modulation of the fluxes with time over the 11-year solar cycle.In particular, the energy spectra in the sub-GeV to TeV range was measured and compared to the predictions of various published flux models. While none of the models were strongly inconsistent with the data, some preference was seen for the HKKM11 model as the most realistic model.The azimuthal analysis measured the east-to-west asymmetry in the neutrino flux, caused by the geomagnetic field, for both flavours at > 5 σ . Measurements were made of the strength of the effect as functions of energy and zenith angle. There was also an indication that the alignment of the asymmetry was dependent on zenith angle, seen at the 2.2 σ level.A search for a long-term correlation between the atmospheric neutrino flux and the solar magnetic activity cycle was performed, however the expected effect based on the HKKM model was calculated to be relatively small. An indication of a correlation was seen at the 1.1 σ level. During particularly strong solar activity events, known as Forbrush decreases, no theoretical prediction is available, but a deviation from the expected neutrino event rate is seen at the 2.4 σ level.

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Determination of the atmospheric neutrino flux and searches for new physics with AMANDA-II

Cited by 98 publications

References 78 publications

Probing particle physics with IceCube

Probing particle physics with IceCube

Interpretation of neutrino flux limits from neutrino telescopes on the Hillas plot

Measurements of the Atmospheric Neutrino Flux at Super-Kamiokande

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