wolfgang rhode- latest results of amanda

8/3/2019 Wolfgang Rhode- Latest Results of AMANDA

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AMANDA


2/22

AMANDA

Latest Resultsof AMANDA

Wolfgang Rhode

Universitt Dortmund

Universitt Wuppertal

for the AMANDA Collaboration


3/22

AMANDA

South Pole

Dark sector

AMANDA

Dome

Runway


4/22

Neutrino Telescope in the Ice

1997:

AMANDA-B10

302 OMs on 10 Strings

2000:

AMANDA-II

677 OMs on 19 Strings


5/22

Single atmospheric Muons

Energy spectrum from

the light depositionDepth intensity relation

1.061.2 =

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


6/22

Cosmic Ray Proton Flux Measurement

Energy spectrum from thelight deposition (QGSJET)Ice property indepent analysis

(H) = 2.70 0.02

0 (H) = 0.106(7) m-2s-1sr-1TeV-104.070.2 =

ICRC 2003: Chirkin for AMANDA ICRC 2003: Geenen for AMANDA


7/22

Multiple Muons and Surface Electrons

preliminary

1 km

2 km

AMAN

DA(numberofmuons)

Spase (number of electrons)

Iron

Proton

log(E/P

eV)

Measurement of the Cosmic RayComposition at the Knee with

SPASE-2 and AMANDA II

400 TeV 6 PeV:

Increase of the Atomic Mass

ICRC 2003: Rawlins for AMANDA & SPASE


8/22

B10: Observation of high-energy atm. neutrinos

AMANDA B 10: 350 /year

Observation of high-energy neutrinos using Cherenkov detectors embedded deep in Antarctic ice,

Ahrens et al., Nature 410, 2001, 441Observation of high energy atmospheric neutrinos with the Antarctic muon and neutrino detector

array, Ahrens et al., Phys. Rev. D. 66, 2002, 012005


9/22

Atmospheric neutrinos with AMANDA II

2000:679

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


10/22

Atmospheric Neutrino Spectrum Measured

with the AMANDA II Detector

Combination of

Neural network constructed energysensitive 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


11/22


12/22

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


13/22

B10 Limit on UHE Muon-Neutrinos

E > 10 PeV: Earth opaque for

neural net cut parameter ->

signal

Signature:~ horizontal UHE events

Background:atm. muon bundles

Limit: 2.5 PeV < E < 5.6 EeV

AMANDA sensitive to upwardhemisphere above 1 PeV

ICRC 2003: Hundertmark for AMANDA


14/22

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

A II

B10

3 Ice

1.19.858.8Cas. A

3.14.941.0Cyg. X-3

1.69.539.8Mkn 501

3.111.238.2Mkn 4212.14.222.0Crab

0.917.012.4M87

0.6-5.0SS433

A IIB 10dec.[deg]Source

declination averaged limit:

lim 2.310-8 cm-2s-1


15/22

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 !


16/22

Search for High Energy Muon Neutrinos

from Gamma-Ray Bursts


17/22

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

AMANDA


18/22

AMANDANew AMANDA-II DAQ

ICRC 2003: Wagner for AMANDA

AMANDA


19/22

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...

AMANDA


20/22

AMANDA

South PoleSouth Pole

Dark sector

AMANDA

IceCubePlanned Location 1 km east

Dome

Skiway

- 80 Strings

- 4800 PMTs

- 1 km3

- 2004 - 2010


21/22

New ReactionsNew Reactions

e + N e- + X + N

- + X

electron cascade

375 TeV 300 m diameter

PeV (300 m)

decays

double bang event

AMANDA


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wolfgang rhode- latest results of amanda

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