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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
Julia Becker October 2005, Como, Italy
Neutrino Physics at the South Pole:
Recent results from the AMANDA experiment
Julia Becker for the IceCube collaboration
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
Julia Becker October 2005, Como, Italy
Astroparticle physics
us
Julia Becker October 2005, Como, Italy
p …
N casc
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)
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
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
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
Julia Becker October 2005, Como, Italy
Diffuse limits and sensitivities
Unfolded spectrum
4yr sensitivity
All flavor limits:Cascades
Ultra High Energies
IceCube
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
Julia Becker October 2005, Como, Italy
Stacking of sources (year 2000)
single source sensitivity (4yrs)
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
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
Julia Becker October 2005, Como, Italy
Average Individual
b
s
'A
FA
ztF
zEss
bb
,,
,
1
1
90
0
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
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
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
