julia becker for the icecube collaboration
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Julia Becker for the IceCube collaboration. Neutrino Physics at the South Pole: Recent results from the AMANDA experiment. Sweden: Uppsala Universitet Stockholm Universitet. UK: Imperial College Oxford University. Netherlands: Utrecht University. Japan: Chiba University. - PowerPoint PPT PresentationTRANSCRIPT
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Julia Becker October 2005, Como, Italy
Neutrino Physics at the South Pole:
Recent results from the AMANDA experiment
Julia Becker for the IceCube collaboration
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Julia Becker October 2005, Como, Italy
USA: Bartol Research Institute University of Alabama Pennsylvania State University University of California – Berkeley University of California – Irvine Clark-Atlanta University University of Maryland Institute for Advanced Study University of Wisconsin-Madison University of Wisconsin-River Falls Lawrence Berkeley National Lab University of Kansas Southern University and A&M
College
In March 2005, AMANDA merged into the IceCube collaboration
Sweden: Uppsala Universitet Stockholm Universitet
UK: Imperial College Oxford University
Netherlands: Utrecht University Belgium:
Université Libre de Bruxelles Vrije Universiteit Brussel Universiteit Gent Université de Mons-Hainaut
Germany: Humboldt Universität Universität Mainz DESY-Zeuthen Universität Dortmund Universität Wuppertal Universität Berlin
Japan: Chiba University
New Zealand: University of Canterbury
Antarctica: Amundsen Scott South Pole Station
AMANDA IceCube
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Julia Becker October 2005, Como, Italy
Astroparticle physics
us
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Julia Becker October 2005, Como, Italy
p …
N casc
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Julia Becker October 2005, Como, Italy
Diffuse Neutrino Spectra
Atmospheric Bg
Extragalactic:AGN (1)
(Becker/Biermann
/Rhode)
AGN (3 and 4)
(Mannheim
/Protheroe/Rachen)
GRBs (2)
(Waxman/Bahcall)
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Julia Becker October 2005, Como, Italy
Amundsen-Scott South Pole Station
South PoleDome
Summer camp
AMANDA
road to work
1500 m
2000 m
[not to scale]
AMANDA/IceCube677 PMTs on 19 strings
Cherencov light
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Julia Becker October 2005, Como, Italy
Detection Strategies
Presented in this talk:Diffuse search
Steady Point sources
Transient objects (AGN flares & GRBs)
WIMPsplus:
SN in our galaxy
Cosmic Ray Composition
Atmospheric muon spectrum
Search for magnetic monopoles
Galactic Plane
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Julia Becker October 2005, Como, Italy
Diffuse energy spectrum
Unfolding the energy spectrum
Data follow atmospheric prediction
Energy spectrum up to 100 TeV
Limit on E-2 extragalactic flux:
11272 106.2 srsGeVcmdE
dNE
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Julia Becker October 2005, Como, Italy
Diffuse limits and sensitivities
Unfolded spectrum
4yr sensitivity
All flavor limits:Cascades
Ultra High Energies
IceCube
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Julia Becker October 2005, Como, Italy
Single sources
Improved background rejection by new pattern recognition method
Blindness strategy: Event selection optimized with randomized RA
Sensitivity (90% C.L.):~ above 10 GeV128106.0 scm
3329 events (2000-2003), mostly atm. neutrinos,< 5% atm. muons
no point source signal seen so far
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Julia Becker October 2005, Como, Italy
Stacking of sources (year 2000)
single source sensitivity (4yrs)
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Julia Becker October 2005, Como, Italy
AGN flares
1. Sliding window: 12 sources tested, no significant excess
2. Multi-wavelength: 3 of the 12 sources, no excess
Mkn421, year 2000
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Julia Becker October 2005, Como, Italy
GRBs – average spectrum
9.5e-7BATSE7400
2.7e-6diffuse search
-01
3e-8BATSE&
IPN
13900-03
4e-8BATSE31297-00
limit/sens.selection
criteria
#(GRB)years
Preliminary
]///[ 2 srscmGeV
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Julia Becker October 2005, Como, Italy
Average Individual
b
s
'A
FA
ztF
zEss
bb
,,
,
1
1
90
0
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Julia Becker October 2005, Como, Italy
GRBs – Individual Spectra
Waxman/Bahcall: average spectrumSingle spectrum approachGRB030329:
Individual par. (model 1,2)
average par. (model 3)
0.0350.036average (WB)
0.0390.041beamed
0.1500.157isotropic
Limit
[GeV/s/cm2]
Sensitivity
[GeV/s/cm2]
Model
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Julia Becker October 2005, Como, Italy
Indirect WIMP search
Dark matter accumulates in high density regions
Earth and Sun: annihilation of WIMPs in the center
If flux from there WIMPS
excluded by
CDMS
● Signal expectation: use Monte Carlo (DARKSUSY)
● No significant excess above background, limit on muon flux
+ -
Results (2001) for solar WIMPs
hard channel: W W
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Julia Becker October 2005, Como, Italy
Summary
AMANDA is an operating UHE neutrino telescopeDifferent search strategies:
Diffuse search, spectrum up to 100 TeV
Steady point sources (single sources & stacking)
Transient sources (flares and GRBs)
Dark matter search
…and more…Analyses show so far no signal above atmospheric fluxConstraints on current models possibleFuture: IceCube