PDD - Atmospheric Neutrinos
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5 Expected IceCube Performance- 5.1 Introduction
- 5.2 Atmospheric Neutrinos
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5.3 Muon-Neutrino-Induced Muons
- 5.3.1 Simulation
- 5.3.2 Reconstruction and Background Rejection
- 5.3.3 Sensitivity to Diffuse Sources of Muon Neutrinos
- 5.3.4 Sensitivity to Muon Neutrino Point Sources
- 5.3.5 Sensitivity to Muon Neutrinos from Gamma-Ray Bursts
- 5.3.6 Possible Improvements
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5.4 Electromagnetic and Hadronic Cascades
- 5.4.1 Simulation
- 5.4.2 Reconstruction
- 5.4.3 Effective Volume
- 5.4.4 Sensitivity to Atmospheric ν
- 5.4.5 Sensitivity to Point Sources
- 5.4.6 Sensitivity to Diffuse νe Sources
- 5.4.7 Sensitivity to GRBs
- 5.4.8 Possible Improvements
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5.5 Tau Neutrinos
- 5.5.1 Tau Neutrino Event Rates
- 5.5.2 Tau Neutrino Simulations
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5.6 Neutrino Flavor Differentiation with Waveform Digitization
- 5.6.1 Photon Flux Distribution Generated by High Energy Cascades
- 5.6.2 ντ Event Signatures
- 5.6.3 Summary
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5.7 Lower Energy Phenomena and Exotica
- 5.7.1 Muon Neutrinos from WIMP annihilation
- 5.7.2 Neutrino oscillations
- 5.7.3 MeV Neutrinos from Supernovae
- 5.7.4 Relativistic magnetic monopoles
- 5.7.5 Slowly moving, bright particles
- 5.8 IceCube Configuration Flexibility
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5.9 Calibration of High-Level Detector Response Variables
- 5.9.1 Geometry Calibration
- 5.9.2 Calibration of Angular Response
- 5.9.3 Calibration of Vertex Resolution
- 5.9.4 Energy Calibration
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5.10 IceTop
- 5.10.1 Tagged Muon Bundles
- 5.10.2 IceTop as a Veto
- 5.10.3 Cosmic-ray Physics
5.2 Atmospheric Neutrinos
The largest contribution to the ν flux from non-transient sources in the energy range of several hundreds of MeV to at least several hundreds of TeV is atmospheric neutrinos. The atmospheric ν flux is dominated by the muon component, increasing from a 2:1 νμ : νe ratio at low energies Eν ∼ 1 GeV to 30:1 at Eν ∼ 100 TeV so that the atmospheric ν "background" to UHE cascades is somewhat smaller than for UHE muons. The following sections will address the use of atmospheric neutrinos as a calibration source at lower energies, and their rejection as a background source at higher energies.
