PDD - IceCube Configuration Flexibility
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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
5.8 IceCube Configuration Flexibility
The default IceCube configuration is optimized for the TeV-PeV neutrino energy region. In the scenario where a potential signal is seen at PeV energies or above, but the IceCube array has not yet been fully deployed, the IceCube design permits considerable flexibility. String deployments can be modified to increase subsequent interstring spacings, expanding the geometrical area at little added financial expense. Since muons at these energies are brighter, one crossing the array would experience no "blind" corridors. Of course, performance at lower energies would suffer with increasing interstring spacing. Conversely, if a signal is detected at the lower end of the TeV-PeV energy scale, the detector can be "backfilled" using as-yet-undeployed DOMs to increase the overall pixel density. This would enhance sensitivity to lower energy neutrinos.
