2009
DOI: 10.1103/physrevd.79.102005
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Determination of the atmospheric neutrino flux and searches for new physics with AMANDA-II

Abstract: The AMANDA-II detector, operating since 2000 in the deep ice at the geographic South Pole, has accumulated a large sample of atmospheric muon neutrinos in the 100 GeV to 10 TeV energy range. The zenith angle and energy distribution of these events can be used to search for various phenomenological signatures of quantum gravity in the neutrino sector, such as violation of Lorentz invariance or quantum decoherence. Analyzing a set of 5511 candidate neutrino events collected during 1387 days of livetime from 2000… Show more

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Cited by 98 publications
(71 citation statements)
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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%
“…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%
“…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%
“…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%