AMANDA

AMANDA

Lessons

Antarctic Muon And Neutrino Detector Array

South Pole, Summer 91/92Muon 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 800-1000 m depth

Sweden joins (Stockholm, Uppsala)

1 km

2 km

93/9440 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 survivefor 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

95/9660

m

AMANDA-B4... and: the first 2 neutrinos!

From ² fit to tailored Likelihood

Scattering

t

far track

close track

0 t

0 t

),,,,,( 0 scattabsiii distttfL

N

i i

ii tt

12

202 )(

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

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 inNATURE, 2001

- 263 neutrino candidates- far from horizon!

1 km

2 km

3 strings instrumented between 1250 -2350 m study deep and shallow ice for future IceCube

Season 97/98

Ice properties vs. depth and wavelength

Scattering Absorption

bubbles

dustdust

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 analogbut 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 problemAmanda: 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 havesolved – even not recognized – theseissues!