AMANDA

AMANDA

Latest Resultsof AMANDA

Wolfgang Rhode

Universität Dortmund

Universität Wuppertal

for the AMANDA Collaboration

AMANDA

South Pole

Dark sector

AMANDA

Dome

Runway

Neutrino Telescope in the Ice

1997:

AMANDA-B10

302 OMs on 10 Strings

2000:

AMANDA-II

677 OMs on 19 Strings

Single atmospheric Muons

ICRC 2003: Desiati for AMANDA ICRC 2003: Geenen for AMANDA

Energy spectrum from the light deposition

Depth intensity relation

• Absolute Flux understood within 30% (CR-Flux*Prim. Int.)

• Energy Spectrum understood within 10% (dEph/dx*PM-Efficiency)

1.061.2

Cosmic Ray Proton Flux Measurement

ICRC 2003: Chirkin for AMANDA ICRC 2003: Geenen for AMANDA

Energy spectrum from the light deposition (QGSJET)Ice property indepent analysis

04.070.2 (H) = 2.70 ± 0.02

0 (H) = 0.106(7) m-2s-1sr-1TeV-1

Multiple Muons and Surface Electrons

ICRC 2003: Rawlins for AMANDA & SPASE

1 km

2 km

preliminary

AM

AN

DA

(nu

mbe

r o

f m

uons

)

Spase (number of electrons)

Iron

Proton

log(E/PeV)Measurement of the Cosmic Ray Composition at the Knee with SPASE-2 and AMANDA II

400 TeV – 6 PeV: Increase of the Atomic Mass

B10: Observation of high-energy atm. neutrinos

Observation of high-energy neutrinos using Cherenkov detectors embedded deep in Antarctic ice, Ahrens et al., Nature 410, 2001, 441

Observation of high energy atmospheric neutrinos with the Antarctic muon and neutrino detector array, Ahrens et al., Phys. Rev. D. 66, 2002, 012005

AMANDA B 10: 350 /year

Atmospheric neutrinos with AMANDA II

2000:679

ICRC 2003: Hauschildt & Steele for AMANDA

horizontal

Sensitivity up to the horizon.

High energy selection in favor of astrophysical neutrinos.

Selection optimized in declination bands.

Atmospheric Neutrino Spectrum Measured with the AMANDA II Detector

ICRC 2003: Geenen for AMANDA

Combination of

•Neural network constructed energy sensitive variable

•Directly measured variables

as input of regularized unfolding

Spectrum up to 100 TeVcompatible with Frejus data

presently no sensitivity to LSND/Nunokawa prediction of dip structures between 0.4-3 TeV

in future: excess studies at high energies

Integral Method: Search for Diffuse Fluxes

ICRC 2003: Hill, Leuthold & Cooley for AMANDA

Limits on Diffuse Fluxes of High Energy Extraterrestrial Neutrinos with the AMANDA-B10 Detector, Ahrens et al., Phys. Rev. Lett. 90, 2003, 251101

Expected sensitivity 2000:~ 3 10-7 GeV-1 cm-2 s-1 sr-1

E2 (E) < 8 10-7

GeV-1 cm-2 s-1 sr-1

Assuming an E-2 spectrum:

Search for High Energy Neutrinos of All Flavorswith AMANDA II

ICRC 2003: Kowalski for AMANDA

Search for neutrino-induced cascades with the AMANDA detector, Ahrens et al., Phys. Rev. D 67, 2003, 012003

Flavor mixing:

Signature: electromagnetic/hadronic cascade within the detector

Limit: 80 TeV < E < 7 PeV

Data: 197 days (2000)

B10 Limit on UHE Muon-Neutrinos

ICRC 2003: Hundertmark for AMANDA

E > 10 PeV: Earth opaque for

Signature: ~ horizontal UHE events

Background: atm. muon bundles

Limit: 2.5 PeV < E < 5.6 EeV neural net cut parameter ->

signal

AMANDA sensitive to upward hemisphere above 1 PeV

Search for extraterrestrial point sources

ICRC 2003: Hauschildt & Steele for AMANDA

Search for Point Sources of high-energy neutrinos with AMANDA, Ahrens et al., Ap. J. 583, 2003, 1040

declination averaged limit:

lim 2.3•10-8 cm-2s-1

Source dec.[deg] B 10 A II

SS433 5.0 - 0.6

M87 12.4 17.0 0.9

Crab 22.0 4.2 2.1

Mkn 421 38.2 11.2 3.1

Mkn 501 39.8 9.5 1.6

Cyg. X-3 41.0 4.9 3.1

Cas. A 58.8 9.8 1.1

A II

B10

3 Ice

Search for Muons from WIMP Annihilation in the Center of the Earth with AMANDA B10

ICRC 2003: Olbrechts for AMANDA

Limits to the muon flux from WIMP annihilation in the center of the Earth with the AMANDA detector, Ahrens et al., Phys. Rev. D, 66 2002, 032006

130 days

DAMA187 days 1999

1997

No WIMP signal observed !

Search for High Energy Muon Neutrinos from Gamma-Ray Bursts

ICRC 2003: Hardtke, Kuehn & Stamatikos for AMANDA

317 BATSE triggers (1997—2000) Limit assuming WB spectrum: 4 x 10-8GeV/s/cm2/sr

<20°

ICRC 2003: Feser for AMANDA

Search for supernova neutrino bursts with the AMANDA detector, Ahrens et al., Astropart. Phys. 16, 2002, 345

B10: 60% of the Galaxy

A-II: 95% of the Galaxy

IceCube: up to LMC

Amanda-II

Amanda-B10

IceCube

0 5 10 sec

Count rates

Search for Neutrino Bursts from Supernovae

AMANDA New AMANDA-II DAQ

ICRC 2003: Wagner for AMANDA

AMANDA

Conclusions

• Improvement of the Analysis• Substantial improvement of the DAQ (2003)• Observed: atm. and • Not observed: HE flux excess, point sources,

GRB, WIMPs, Monopoles, SN, SNR...• Best limits on additional processes• Exclusion of theoretical models• IceCube...

AMANDA

South PoleSouth Pole

Dark sector

AMANDA

IceCubePlanned Location 1 km east

Dome

Skiway

- 80 Strings- 4800 PMTs - 1 km3

- 2004 - 2010

AMANDA