latest results of amanda
DESCRIPTION
Latest Results of AMANDA. Wolfgang Rhode Universität Dortmund Universität Wuppertal for the AMANDA Collaboration. South Pole. Dark sector. Runway. AMANDA. Dome. Neutrino Telescope in the Ice. 1997: AMANDA-B10 302 OMs on 10 Strings 2000: AMANDA-II 677 OMs on 19 Strings. - PowerPoint PPT PresentationTRANSCRIPT
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AMANDA
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AMANDA
Latest Resultsof AMANDA
Wolfgang Rhode
Universität Dortmund
Universität Wuppertal
for the AMANDA Collaboration
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AMANDA
South Pole
Dark sector
AMANDA
Dome
Runway
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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
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
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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
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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
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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
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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.
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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
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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:
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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)
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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
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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
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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 !
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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°
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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
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AMANDA New AMANDA-II DAQ
ICRC 2003: Wagner for AMANDA
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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...
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AMANDA
South PoleSouth Pole
Dark sector
AMANDA
IceCubePlanned Location 1 km east
Dome
Skiway
- 80 Strings- 4800 PMTs - 1 km3
- 2004 - 2010
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AMANDA