AMANDA Lessons Antarctic Muon And Neutrino Detector Array

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

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

Deploy 4 strings at m depth

Sweden joins (Stockholm, Uppsala)

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

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!

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!

 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)

Vic Stenger (DUMAND): This is what Amanda sees

F.H.: and this is what DUMAND sees

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

1995: DESY joins

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

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

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

1 km 2 km 96/97 AMANDA - B 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

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

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

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

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

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

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

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 !

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

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

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

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

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

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

Challenges

The bubble problem Amanda: to be or not to be

The ice challenge Kurt

Reconstructing tracks

The gain drop problem

The stuck string

Finding the best technology

Without AMANDA, we would not have solved – even not recognized – these issues!