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AMANDA: Antarctic Muon and Neutrino Detector Array Lessons

Explore the history, data, and advancements of the AMANDA project, including challenges faced and solutions found. From early beginnings at the South Pole to breakthroughs in neutrino detection capabilities, the journey of AMANDA is a testament to scientific innovation. Learn about key milestones, collaborations, and discoveries that have shaped our understanding of cosmic phenomena.

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AMANDA: Antarctic Muon and Neutrino Detector Array Lessons

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  1. AMANDA AntarcticMuonAndNeutrinoDetectorArray Lessons Christian Spiering

  2. South Pole, Summer 91/92 Muon rates consistent with 25 m absorption length

  3. Bruce Koci ( 2006) Francis Halzen: The success of AMANDA stood on two pillars: the Amundsen Scott Station and Bruce Koci.

  4. 1993 Deploy 4 strings at 800-1000 m depth

  5. South Pole 93/94 AMANDA-A Sweden joins (Stockholm, Uppsala)

  6. AMANDA-A 93/94 40 m 1 km CATASTROPHAL DELAY OF LIGHT ! 2 km

  7. February 94: Amanda measures delay • March 94, Venice: G. Domogatsky points to Vostok results: it is scattering by remnant air bubbles ! • April 94: tendency confirmed by Amanda data! Vostok Data

  8. February 94: Amanda measures delay • March 94, Venice: G. Domogatsky points to Vostok results: it is scattering by remnant air bubbles ! • April 94: tendency confirmed by Amanda data! Vostok Data

  9. February 94: Amanda measures delay • March 94, Venice: G. Domogatsky points to Vostok results: it is scattering by remant air bubbles ! • April 94: tendency confirmed by Amanda data! (delay time of light)

  10. Vic Stenger (DUMAND): This is what Amanda sees

  11. F.H.: and this is what DUMAND sees

  12. 1 km 2 km Can detect Supernovae with non-tracking detector! Detector works very stable Lousy scattering length ~ 1m, but: absorption length ~ 200 m ! 40 m Supernova detection No tracking. But photons survive for long time

  13. 1995: DESY joins

  14. AMANDA-B4 1 km 2 km •  no bubbles left • scattering now dominated by dust •  average scattering length ~ 25 m •  average absorption length >100 m • down to wavelength of 337 nm ! 95/96 60 m

  15. AMANDA-B4 1 km 2 km ... and: the first 2 neutrinos! 95/96 60 m

  16. From ² fit to tailored Likelihood t 0t Scattering far track close track 0t

  17. 96/97 AMANDA - B10 1 km 2 km ~300 neutrino events separated from 1997 data (~ 6 months)  first physics  intensive learning period on ice dust layers as well as hole ice 6 additional strings 120 m

  18. 96/97 AMANDA - B10 1 km 2 km IceCube will work ! The EVA event 120 m

  19. 96/97 AMANDA - B10 1 km 2 km B10 skyplot published in NATURE, 2001 - 263 neutrino candidates - far from horizon! 120 m

  20. Season 97/98 1 km 2 km  3 strings instrumented between 1250 -2350 m  study deep and shallow ice for future IceCube

  21. Ice properties vs. depth and wavelength Scattering Absorption bubbles ice dust dust

  22. Factor 2 gain loss in several months ! 1 km 2 km The gain-drop problem • Lessons: • Need rigid long term tests • Selection of components • - Lower HV

  23. 1999/2000 AMANDA-II 1 km Nearly horizontal  2 km  total of 19 strings with 677 PMTs  greatly enhanced sensitivity at horizon  angular resolution ~ 2 degrees  test IceCube technology (string 18) 200 m

  24. 1999/2000 AMANDA-II 1 km 2 km Alas! The stuck string • Lesson: • - Fast is good. Too fast is bad. • More careful optimization of • drilling regime !

  25. 1 km 2 km Use SPASE for pointing studies SPASE air shower arrays  resolution Amanda-B10 ~ 3°  absolute pointing < 1.5° results in ~ 2.5° for upward moving muons

  26. Evolution of read-out strategy Test of IC3 technology - timing - dyn. range - no x-talk • - cost • - robustness • - dyn. range • easy • calibration

  27. dAOM versus DOM dAOM (DESY) DOM (LBNL) copper cable digital optical fibre analog but a) HV in OM b) PM-anode  amplifier  LED (dynamic range!)

  28. Lesson: take the best and then collaborate! • in ice: DOM (Digital Optical Module): LBNL • at surface: DOR (DOM Receiver Card): DESY

  29. AMANDA = 30 x SuperK, MACRO (AMANDA = 1/30 IceCube)

  30. AMANDA 7 years: The results • 6595 neutrinos up to record energy of 200 TeV • Record limits on fluxes for cosmic neutrinos (diffuse, point sources, GRB) • Record limits on indirect dark matter search, magnetic monopoles, tests of Lorentz invariance • Monitoring the galaxy for supernova bursts • Spectrum and composition of cosmic rays

  31. Challenges

  32. The bubble problem Amanda: to be or not to be

  33. The ice challenge Kurt

  34. Reconstructing tracks

  35. The gain drop problem

  36. The stuck string

  37. Finding the best technology

  38. Without AMANDA, we would not have solved – even not recognized – these issues! Well done AMANDA!

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