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AMANDA and IceCube neutrino telescopes at the South Pole

AMANDA and IceCube neutrino telescopes at the South Pole. Per Olof Hulth Stockholm University. Members of the AMANDA SU group. Senior members Christian Bohm Per Olof Hulth Klas Hultqvist Christian Walck Forskarassistent Stephan Hundertmark Resarch students Thomas Burgess

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AMANDA and IceCube neutrino telescopes at the South Pole

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  1. AMANDA and IceCube neutrino telescopes at the South Pole Per Olof Hulth Stockholm University

  2. Members of the AMANDA SU group • Senior members • Christian Bohm • Per Olof Hulth • Klas Hultqvist • Christian Walck • Forskarassistent • Stephan Hundertmark • Resarch students • Thomas Burgess • Patrik Ekström (Wuppertal) • Yulia Minaeva • Julio Rodriguez Martino • Christin Wiedemann • Electronic engenieer • Lars Thollander

  3. Scientific goal • Detect High Energy cosmic neutrinos by using the ice sheet at The South Pole as a target. • Method: Detect the emitted Cherenkov light from neutrino induced interactions in the ice.

  4. Activities • Mainly analysis and software development • Preamplifiers designed and built in Stockholm (SWAMPS)

  5. Neutrino interaction   < 1 degree The muon can travel several km in e.g. ice

  6. South Pole Dark sector Skiway AMANDA Dome IceCube

  7. myon neutrino

  8. Hot water heaters -50 m -55 C 1400 m -42C -20 C -2400 m

  9. Photomultipliers: Hamamatsu 20 cm 14 dynodes Gain 109

  10. AMANDA electronics • Three different cable types (2400 -2600 m) • Strings 1-4 coax cable, rise time 250 ns • Strings 5-10 twisted pair rise time, 50-70 ns • Strings 11-19 twisted pair rise time 100-150 ns • Analog signal at surface about 1-10 mV • Amplified 100 times by Stockholm “SWAMP” (Lars Thollander)

  11. Technical requirements • Absolute timing <7 ns from any OM • Geometrical position uncertainty < 1m • Electronic in ice should stand -50 C • Low noise

  12. Building AMANDA: The Optical Module and the String

  13. - timing - dyn. range - no x-talk - easy calibration - cost - robustness - dynamic range Evolution of read-out strategy Strings 1-10 Strings 11-17,19 String 18

  14. New Project IceCube • Increase volume to 1 km3 • 80 strings with 60 modules each • Photomultiplier 25 cm (10 inch) 10 dynodes (preliminary Hamamatsu) • Air shower detector on top (IceTop) • Transport drill to Pole 03/04 • First 1-7 strings in 04/05

  15. IceTop AMANDA South Pole IceCube Skiway 80 Strings 4800 PMT 1400 m 2400 m

  16. Grid North 100 m AMANDA South Pole SPASE-2 Dome Skiway IceCube:Top View 80 strings 60 modules/string Volume 1 km3 Depth 1400-2400 m Counting House

  17. µ-events in IceCube Eµ=6 PeV Eµ=10 TeV AMANDA-II 1 km Measure energy by counting the number of fired PMT. (This is a very simple but robust method)

  18. Self-triggers on each pulse Captures waveforms Time-stamps each pulse Digitizes waveforms Performs feature extraction Buffers data Responds to Surface DAQ Set PMT HV, threshold, etc Noise rate in situ: ≤500 Hz 1. Digital Optical Module DOM 33 cm

  19. IceCube String 1400 m OM Spacing: 17 m 2400 m

  20. Experimental Requirements IceCube • Time resolution: <5 ns rms • Waveform capture: >250 MHz -for first 500 ns ~40 MHz -for 5000 ns • Dynamic Range: >200 PE / 15 ns >2000 PE / 5000 ns • Dead-time: < 1% • OM noise rate: < 500 Hz(40K in glass sphere)

  21. 2. DAQ Network architecture

  22. In-Door deployment

  23. ENGINEERING AND INSTRUMENTATION MADISON UNIVERSITY OF WISCONSIN - Hose Winch for the Ice Cube Project

  24. Receiving drum weldment

  25. POSITION OF DRILL(30HOUR ANALYSIS)

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