PowerPoint-Pr

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Recent Results
Lutz Köpke University of Mainz, Germany July 31,
2003
http//amanda.uci.edu
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Contributed papers to ICRC
? Response of AMANDA to cosmic ray muons ? Cosmic
ray flux measurement ? Cosmic ray composition at
the knee with SPASE and AMANDA ? Atmospheric
neutrino and muon spectra ? Search for diffuse
fluxes of extraterrestrial muon neutrinos ?
AMANDA-B10 limit on UHE-Neutrinos ? Search for
high energy neutrinos of all flavours ? Search
for extraterrestrial point sources of neutrinos ?
Search for muons from WIMP annihilation in center
of earth ? Search for high energy neutrinos from
GRBs ? Online search for neutrino bursts from
Supernovae ? New capabilities of the AMANDA
detector ? The IceCube high energy neutrino
telescope ? IceTop the surface component of
IceCube ? Simulation of ice Cherenkov detectors
for IceTop
3 individual contributions
black parallel talk
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Physics motivation

• ? origin and acceleration of cosmic rays
• ? understand cosmic cataclysms
• ? find new kind of objects?
• ? neutrino properties (?? , cross sections ..)
• ? dark matter (neutralino annihilation)
• tests of relativitiy ....
• search for big bang relics ...
• effects of extra dimension etc. ...

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Neutrino source candidates
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Importance of all flavor detection
Extended source with ?e???? 120 production
(e.g. ?? decay) Expect for Maki-Nakagawa-Sakato
mixing matrix with ?1230, ?2345, ?130
?e???? 111 on earth
? O(10) x less background for ?e but you dont
profit from long ?-range ? Regeneration of ?? -
no absorption in earth even at very high energies
!
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Detection of ?e ,?? , ??
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Detection of muon neutrinos
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Complementarity (point sources)
E ?lt 100 TeV
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Northern hemisphere detectors
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AMANDA II Detector
Amundsen-Scott Station South Pole
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The AMANDA Collaboration
? 150 members

• Bartol Research Institute
• UC Berkeley
• UC Iivine
• Pennsylvania State
• UW Madison
• UW River Falls
• LBL Berkeley
• U. Simón Bolivar, Caracas
• VUB, Brussel
• ULB-IHEE, Bruxelles
• U. de Mons-Hainaut
• Imperial College, London
• DESY, Zeuthen
• Mainz Universität
• Wuppertal Universität
• Stockholm Universitet
• Uppsala Universitet
• Kalmar Universitet
• South Pole Station Antarctica

Antarctica
New Zealand
Venezuela (1)
USA (73)
Europe (101)
Japan
associated institutes e.g. Chiba University
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The laboratory
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The new station operating at least until 2035
The Dome
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Two events ...
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Detector capabilities
? muons directional error 2.0 - 2.5 energy
resolution 0.3 0.4 coverage 2? ?
primary cosmic rays ( SPASE) energy
resolution 0.07 0.10 ? cascades (e, ??
, neutral current) zenith error 30 - 40
energy resolution 0.1 0.2 coverage 4?
?log10(E/TeV)
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Atmospheric muons in AMANDA-II
poster 1-P-265
Atmospheric muons and neutrinos AMANDAs test
beams
much improved simulation ...but data 30 higher
than MC ... ? normalize to most vertical
bin Systematic errors ? 10 scattering (
20m _at_ 400nm) absorption (110m _at_
400nm) ? 20 optical module sensitivity ? 10
refreezing of ice in hole
PRELIMINARY
threshold energy 40 GeV (zenith averaged)
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Cosmic Ray flux measurement
talk HE2.1-13
In some cases ice and OM-sensitivity effect can
be circumvented ...

• ?(E)?0E-?

empirical separation of ice and OM sensitivity
effects
PRELIMINARY
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cosmic ray composition studies
talk HE 1.1-25
SPASE-2 (electronic component) - AMANDA B10
(muonic component)
- unique combination!
AMANDA II
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talk HE 1.1-25
Composition change around knee
1015 eV
1016 eV
A30
A6
publication in preparation
1998 data
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Atmospheric n's in AMANDA-II
talk HE 2.3-6
? neural network energy reconstruction ?
regularized unfolding
PRELIMINARY
measured atmospheric neutrino spectrum
1 sigma energy error
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Excess of cosmic neutrinos? Not yet ...
talk HE 2.3-4
poster HE
.. for now use number of hit channels as energy
variable ...
muon neutrinos (1997 B10-data) accepted by PRL
AGN with 10-5 E-2 GeV-1 cm-2 s-1 sr-1
cuts determined by MC blind analyses !
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Diffuse flux muon neutrinos
poster 1-P-257
poster 1-P-256
Note that limits depend on assumed energy
spectrum ...
3103 106 GeV E2 ?(E) lt 8 ?10-7 GeV-1 cm-2
s-1 sr-1

prel.
2.5 106 5.6 108 GeV E2 ?(E) lt 7.2 ?10-7
GeV-1 cm-2 s-1 sr-1
AMANDA II (with 3 years data) 10 X higher
Sensitivity
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Diffuse limit cascades
talk HE 2.3-4
Effective volume
80 TeV 7 PeV
PRELIMINARY
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Flux results summary (all flavors)
talk HE 2.3-4
assuming ?e???? 111 ratio
? special analysis for resonant
production (6.3 PeV) ? multiplicative factor 3
applied for single ?e ,?? channels
...can combine analyses!
2000 ?? analysis will yield comparable result ...
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Theoretical bounds and future
opaque for neutrons
MPR
neutrons can escape
atmospheric ??
WB
Mannheim, Protheroe and Rachen (2000) Waxman,
Bahcall (1999) ? derived from known limits on
extragalactic protons ?-ray flux
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Point source search in AMANDA II
talk HE 2.3-5
Search for excess events in sky bins for up-going
tracks
PRELIMINARY
? 697 events observed above horizon ? 3
non-neutrino background for ? gt 5 ? cuts
optimized in each declination band
no clustering observed - no evidence for
extraterrestrial neutrinos ...
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talk HE 2.3-5
Selected point source flux limits
sensitivity ? flat above horizon - 4 times
better than B10 !
PRELIMINARY
Sources declination 1997 2000
SS433 5.0o - 0.7
M87 12.4o 17.0 1.0
Crab 22.0o 4.2 2.4
Mkn 421 38.2o 11.2 3.5
Mkn 501 39.8o 9.5 1.8
Cyg. X-3 41.0o 4.9 3.5
Cas. A 58.8o 9.8 1.2
declination averaged sensitivity ??lim ?
0.2310-7 cm-2s-1 _at_90
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N
Expected source sensitivity
muons/cm2 s1
AMANDA 137 days
10-14
S
MACRO 8 years
published data
10-15
10-16
10-17
declination (degrees)
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GRB n search in AMANDA
talk OG 2.4-7
Search for ?? candiates correlated with GRBs -
background established from data
??lt20
PRELIMINARY
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Outlook
... did not mention new improved search for WIMPs
(HE 3.3-6) ... supernova detection (1-P-258) etc.

• combined analysis 1997-2003 8 x more days !
• ? improved selection and analysis methods ...
• ? new transition waveform based readout installed
  02/03
• improved performance in particular at high
  energies (1-P-264)
• ? first IceCube strings 2004/05 combined
  analysis with AMANDA

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Is there a signal at higher energies?
no indication of clustering also at higher
energies !
increasing energy deposition
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Sun
Crab Nebula
Cassiopeia. A
LMC
Cygnus-X1
SMC
Approximate AMANDA horizon
90 000 light years