PowerPointPrsentation

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Latest Resultsof AMANDA

• Wolfgang Rhode
• Universität Dortmund
• Universität Wuppertal
• for the AMANDA Collaboration

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South Pole
Dark sector
Runway
AMANDA
Dome
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Neutrino Telescope in the Ice
1997 AMANDA-B10 302 OMs on 10
Strings 2000 AMANDA-II 677 OMs on 19 Strings
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Single atmospheric Muons
Energy spectrum from the light deposition
Depth intensity relation

• Absolute Flux understood within 30
  (CR-FluxPrim. Int.)
• Energy Spectrum understood within 10
  (dEph/dxPM-Efficiency)

ICRC 2003 Desiati for AMANDA
ICRC 2003 Geenen for AMANDA
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Cosmic Ray Proton Flux Measurement
Energy spectrum from the light deposition (QGSJET)
Ice property indepent analysis
? (H) 2.70 0.02 ?0 (H) 0.106(7)
m-2s-1sr-1TeV-1
ICRC 2003 Chirkin for AMANDA
ICRC 2003 Geenen for AMANDA
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Multiple Muons and Surface Electrons
preliminary
Measurement of the Cosmic Ray Composition at the
Knee with SPASE-2 and AMANDA II 400 TeV 6 PeV
Increase of the Atomic Mass
ICRC 2003 Rawlins for AMANDA SPASE
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B10 Observation of high-energy atm. neutrinos
AMANDA B 10 350 m/year
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
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Atmospheric neutrinos with AMANDA II
2000679 m
horizontal
Sensitivity up to the horizon. High energy
selection in favor of astrophysical
neutrinos. Selection optimized in declination
bands.
ICRC 2003 Hauschildt Steele for AMANDA
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Atmospheric Neutrino Spectrum Measured with the
AMANDA II Detector

• Combination of
• Neural network constructed energy sensitive
  variable
• Directly measured variables
• as input of regularized unfolding

Spectrum up to 100 TeV compatible 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
ICRC 2003 Geenen for AMANDA
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Integral Method Search for Diffuse Fluxes
Assuming an E-2 spectrum
E2 ?(E) lt 8 ?10-7 GeV-1 cm-2 s-1 sr-1
Expected sensitivity 2000 3 ?10-7 GeV-1 cm-2
s-1 sr-1
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
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Search for High Energy Neutrinos of All
Flavorswith AMANDA II
Flavor mixing
Signature electromagnetic/hadronic cascade
within the detector
Data 197 days (2000)
Limit 80 TeV lt E lt 7 PeV
ICRC 2003 Kowalski for AMANDA Search for
neutrino-induced cascades with the AMANDA
detector, Ahrens et al., Phys. Rev. D 67, 2003,
012003
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B10 Limit on UHE Muon-Neutrinos
E gt 10 PeV Earth opaque for nm
Signature horizontal
UHE nm events Background atm.
muon bundles Limit 2.5 PeV lt E lt 5.6 EeV
signal
neural net cut parameter -gt
AMANDA sensitive to upward hemisphere above 1 PeV
ICRC 2003 Hundertmark for AMANDA
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Search for extraterrestrial point sources
declination averaged limit ??lim ? 2.310-8
cm-2s-1
B10
A II
3 Ice
ICRC 2003 Hauschildt Steele for AMANDA Search
for Point Sources of high-energy neutrinos with
AMANDA, Ahrens et al., Ap. J. 583, 2003, 1040
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Search for Muons from WIMP Annihilation in the
Center of the Earth with AMANDA B10
No WIMP signal observed !
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
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Search for High Energy Muon Neutrinos from
Gamma-Ray Bursts
??lt20
317 BATSE triggers (19972000) Limit
assuming WB spectrum 4 x
10-8GeV/s/cm2/sr
ICRC 2003 Hardtke, Kuehn Stamatikos for AMANDA
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Search for Neutrino Bursts from Supernovae
Amanda-II
Amanda-B10
B10 60 of the Galaxy A-II 95 of the
Galaxy IceCube up to LMC
IceCube
ICRC 2003 Feser for AMANDA Search for supernova
neutrino bursts with the AMANDA detector, Ahrens
et al., Astropart. Phys. 16, 2002, 345
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New AMANDA-II DAQ
ICRC 2003 Wagner for AMANDA
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Conclusions

• Improvement of the Analysis
• Substantial improvement of the DAQ (2003)
• Observed atm. m and n
• Not observed HE flux excess, point sources, GRB,
  WIMPs, Monopoles, SN, SNR...
• Best limits on additional processes
• Exclusion of theoretical models
• IceCube...

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South Pole

• - 80 Strings
• - 4800 PMTs
• 1 km3
• 2004 - 2010

Dark sector
Skiway
AMANDA
Dome
IceCube
Planned Location 1 km east
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New Reactions
ne N ? e- X
nt N? t- X

• electron cascade
• 375 TeV 300 m diameter

double bang event
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