Preliminary Design Document by Section

By Section | Whole Paper | PDF (233 pages, ~6.62mb)

• Introduction
• 1 Document Overview
• 2 Executive Summary
• 3 Science Motivation for Kilometer-Scale Detectors
  • 3.1 High-Energy Neutrinos Associated with Cosmic Particle Accelerators
    • 3.1.1 Energy Considerations
    • 3.1.2 Estimates Based on Models
    • 3.1.3 Neutrinos as a Diagnostic of TeV Gamma-Ray Sources
  • 3.2 Other Science Opportunities
    • 3.2.1 WIMPs and Other Sources of Sub-TeV ν_μ
    • 3.2.2 Atmospheric Neutrinos
    • 3.2.3 PeV and EeV Neutrinos
    • 3.2.4 Tau Neutrino Detection
    • 3.2.5 Neutrinos from Supernovae
  • 3.3 Summary
• 4 Status of High Energy Neutrino Astronomy
  • 4.1 Status of AMANDA
    • 4.1.1 Atmospheric Neutrinos
    • 4.1.2 Pointing Resolution
    • 4.1.3 Search for a diffuse high energy neutrino
    • 4.1.4 Point Sources
    • 4.1.5 Gamma-Ray Bursts
    • 4.1.6 WIMPs
    • 4.1.7 Supernovae
    • 4.1.8 Magnetic Monopoles
    • 4.1.9 Summary of AMANDA Status
• 5 Expected IceCube Performance
  • 5.1 Introduction
  • 5.2 Atmospheric Neutrinos
  • 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
  • 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 ν_e Sources
    • 5.4.7 Sensitivity to GRBs
    • 5.4.8 Possible Improvements
  • 5.5 Tau Neutrinos
    • 5.5.1 Tau Neutrino Event Rates
    • 5.5.2 Tau Neutrino Simulations
  • 5.6 Neutrino Flavor Differentiation with Waveform Digitization
    • 5.6.1 Photon Flux Distribution Generated by High Energy Cascades
    • 5.6.2 ν_τ Event Signatures
    • 5.6.3 Summary
  • 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
  • 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
  • 5.10 IceTop
    • 5.10.1 Tagged Muon Bundles
    • 5.10.2 IceTop as a Veto
    • 5.10.3 Cosmic-ray Physics
• 6 Experimental Requirements
  • 6.1 Time Resolution
  • 6.2 Waveforms
  • 6.3 Dynamic Range and Linearity
  • 6.4 Absolute Amplitude Calibration and Stability
  • 6.5 Dead time
  • 6.6 Sensitivity of optical modules
  • 6.7 Noise Rate and Noise Rate Stability
  • 6.8 Failure Rate
  • 6.9 IceTop
• 7 Design and Description of IceCube
  • 7.1 Overview
  • 7.2 Digital Optical Module
    • 7.2.1 Pressure Housing
    • 7.2.2 Optical Sensor
    • 7.2.3 PMT HV Generator
    • 7.2.4 Optical Beacon
    • 7.2.5 Signal Processing Circuitry
    • 7.2.6 Local/Global Time Transformation
    • 7.2.7 Cable Electrical Length Measurement
    • 7.2.8 Data Flow and Feature Extraction
    • 7.2.9 Local Coincidence
    • 7.2.10 System Design Aspects
  • 7.3 Network
    • 7.3.1 Copper Links
    • 7.3.2 Time-Base Distribution
  • 7.4 Surface DAQ
    • 7.4.1 Overview
    • 7.4.2 DOM Hub
    • 7.4.3 String Processor
    • 7.4.4 IceCube and IceTop System Integration
    • 7.4.5 Experiment and Configuration Control
    • 7.4.6 Security Environment
    • 7.4.7 DAQ Components
    • 7.4.8 Calibration Operations
    • 7.4.9 DAQ and Online Monitoring
    • 7.4.10 DAQ Computing Environment
  • 7.5 AMANDA Data Transmission Techniques
• 8 Data Handling
  • 8.1 System Elements
    • 8.1.1 Software Management
    • 8.1.2 System Engineering
    • 8.1.3 Development Environment
    • 8.1.4 Analysis Framework
    • 8.1.5 Database
    • 8.1.6 Visualization
    • 8.1.7 Development Interfaces
    • 8.1.8 Integration at Pole
    • 8.1.9 Hardware
    • 8.1.10 Data Distribution
  • 8.2 Offline Data Flow
  • 8.3 Data Model
    • 8.3.1 High Multiplicity
    • 8.3.2 Upgoing Tracks
    • 8.3.3 Cascades/Taus
    • 8.3.4 GRB Downgoing Muons
    • 8.3.5 Icetop
    • 8.3.6 Supernova
    • 8.3.7 Prescaled Raw Data
    • 8.3.8 Monitor
    • 8.3.9 Calibration
    • 8.3.10 Full-Sky Summary Histograms
    • 8.3.11 Unfiltered Raw
  • 8.4 Data Sample Organization
  • 8.5 Latency
  • 8.6 Schedule
  • 8.7 Summary
• 9 Data Analysis
  • 9.1 Introduction
  • 9.2 Analysis Infrastructure
    • 9.2.1 Calibration Analysis and Data Quality Working Group
    • 9.2.2 Simulation Working Group
    • 9.2.3 Reconstruction Working Group
  • 9.3 Computing Infrastructure
  • 9.4 Physics Analysis
  • 9.5 Internal Review Procedure
    • 9.5.1 Introduction
    • 9.5.2 Procedure
  • 9.6 Prerequisites and Schedule
• 10 Drilling, Deployment and Logistics
  • 10.1 Drilling
    • 10.1.1 Introduction
    • 10.1.2 Evolution of AMANDA Drills
    • 10.1.3 Performance Criteria and Design of the EHWD
  • 10.2 Deployment
    • 10.2.1 Overview
    • 10.2.2 AMANDA Experience
    • 10.2.3 AMANDA Deployment
    • 10.2.4 IceCube Deployment Overview
    • 10.2.5 IceCube String Deployment Procedure
    • 10.2.6 IceCube Indoor Deployment
    • 10.2.7 IceCube Drill Hole Requirements
    • 10.2.8 Quality Assurance
    • 10.2.9 Practice Deployments
    • 10.2.10 Surface Cable Installation
  • 10.3 Logistics
    • 10.3.1 Introduction
    • 10.3.2 Documentation
    • 10.3.3 Personnel and Taskings
    • 10.3.4 Medical/Dental Examinations
    • 10.3.5 Airline Travel
    • 10.3.6 Weights and Cubes
    • 10.3.7 Cargo Transport
• 11 Quality Assurance
• 12 Relationship of AMANDA and IceCube
• References