AMANDA
AMANDA
Latest Results
of AMANDA
Wolfgang Rhode
Universität Dortmund
Universität Wuppertal
for the AMANDA Collaboration
AMANDA
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
Single atmospheric Muons
Depth intensity relation
Energy spectrum from
the light deposition
  2.61  0.1
• Absolute Flux understood within 30%
(CR-Flux*Prim. Int.)
• Energy Spectrum understood within 10% (dEph/dx*PM-Efficiency)
ICRC 2003: Desiati for AMANDA
ICRC 2003: Geenen for AMANDA
Cosmic Ray Proton Flux Measurement
Ice property indepent analysis
 (H) = 2.70 ± 0.02
0 (H) = 0.106(7) m-2s-1sr-1TeV-1
ICRC 2003: Chirkin for AMANDA
Energy spectrum from the
light deposition (QGSJET)
  2.70  0.04
ICRC 2003: Geenen for AMANDA
1 km
2 km
AMANDA (number of muons)
Multiple Muons and Surface Electrons
Iron
Proton
Spase (number of electrons)
ICRC 2003: Rawlins for AMANDA & SPASE
Measurement of the Cosmic Ray
Composition at the Knee with
SPASE-2 and AMANDA II
400 TeV – 6 PeV:
of the Atomic Mass
Increase
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
Atmospheric neutrinos with AMANDA II
2000:679 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
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
Integral Method: Search for Diffuse Fluxes
Assuming an E-2 spectrum:
E2 (E) < 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
Search for High Energy Neutrinos of All Flavors
with AMANDA II
Flavor mixing:
Signature:
electromagnetic/hadronic cascade
within the detector
Data: 197 days (2000)
Limit: 80 TeV < E < 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
B10 Limit on UHE Muon-Neutrinos
E > 10 PeV: Earth opaque for nm
Signature:
~ horizontal UHE nm events
Background:
atm. muon bundles
signal
Limit: 2.5 PeV < E < 5.6 EeV
neural net cut parameter ->
AMANDA sensitive to upward
hemisphere above 1 PeV
ICRC 2003: Hundertmark for AMANDA
Search for extraterrestrial point sources
declination averaged limit:
nlim  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
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
Search for Muons from WIMP Annihilation in
the Center of the Earth with AMANDA B10
130 days
DAMA
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
1997
187 days
1999
Search for High Energy Muon Neutrinos
from Gamma-Ray Bursts
<20°
Year #GRB
1997
78
1998
99
1999
96
2000
44
Total 317
bkg
0,06
0,20
0,20
0,83
1,29
observed
0
0
0
0
0
317 BATSE triggers (1997—2000)
Limit assuming WB spectrum:
4 x 10-8GeV/s/cm2/sr
ICRC 2003: Hardtke, Kuehn & Stamatikos for AMANDA
Search for Neutrino Bursts from Supernovae
Count rates
Amanda-II
Amanda-B10
0
5
10 sec
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.,
Phys. 16, 2002, 345
Astropart.
AMANDA
New AMANDA-II DAQ
ICRC 2003: Wagner for AMANDA
AMANDA
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...
AMANDA
- 80 Strings
- 4800 PMTs
- 1 km3
- 2004 - 2010
South Pole
Dark sector
Skiway
AMANDA
Dome
IceCube
Planned Location 1 km east
AMANDA