1. AMANDA Lessons Antarctic Muon And Neutrino Detector Array

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

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

4. Deploy 4 strings at 800-1000 m depth

5. Sweden joins (Stockholm, Uppsala)

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

7. Vostok Data  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!

8. Vostok Data  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!

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

13. 1995: DESY joins

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

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

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

17. 1 km 2 km 96/97 AMANDA - B10 120 m  ~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

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

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

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

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

22. 1 km 2 km Lessons: - Need rigid long term tests - Selection of components - Lower HV The gain-drop problem

23. 1 km 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 Nearly horizontal  1999/2000 AMANDA-II

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

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

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

27. dAOM versus DOM 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!