AMANDA Neutrino Astronomy at the South Pole

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AMANDANeutrino Astronomy at the South Pole
Christian Spiering Paris, June
2004
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The AMANDA Collaboration
7 US, 10 European and 1 South American
institution, 110 members Bartol
Research Institute, University of Delaware,
Newark, USA BUGH Wuppertal, Germany Universite
Libre de Bruxelles, Brussels, Belgium Universidad
Simon Bolivar, Caracas, Venezuela DESY-Zeuthen,
Zeuthen, Germany Dept. of Technology, Kalmar
University, Kalmar, Sweden Lawrence Berkeley
National Laboratory, Berkeley, USA Dept. of
Physics, UC Berkeley, USA Institute of Physics,
University of Mainz, Mainz, Germany University of
Mons-Hainaut, Mons, Belgium University of
California, Irvine, CA Dept. of Physics,
Pennsylvania State University, University Park,
USA Physics Department, University of Wisconsin,
River Falls, USA Physics Department, University
of Wisconsin, Madison, USA Division of High
Energy Physics, Uppsala University, Uppsala,
Sweden Fysikum, Stockholm University, Stockholm,
Sweden Vrije Universiteit Brussel, Brussel,
Belgium Imperial College, London, United Kingdom
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Cosmic Rays
Emax ? ? B ? L
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Supernovae shock waves into
interstellar medium
up to 1016 eV
Crab Nebula
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Active Galaxies Accretion Disks and Jets
up to 1020 eV
VLA image of Cygnus A
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Neutrino-Telescopes in Water and Ice
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Antarctic Muon And Neutrino Detector Array
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Antarktis
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C-130
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Mount Erebus
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MACMURDO
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Amundsen und Scott 1911/12
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Areal View
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AMANDA
South Pole
Dome
Summer camp
1500 m
Amundsen-Scott South Pole station
2000 m
not to scale
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Old and new station
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Amanda
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Counting House
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AMANDA-II
677 optical modules at 19 strings
Installation 1996-2000
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Drilling
Hot water drilling
2 MW power 3-4 days / 2 km
60 cm hole
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AMANDA Event SignaturesMuons
CC muon neutrino interaction ? track
nm N ? m X
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AMANDA Event Signatures Cascades

• CC electron and tau neutrino interaction
• ?(e,?,) N ? (e, ?) X
• NC neutrino interaction
• ?x N ? ?x X

Cascades
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Point source search
Atmospheric Neutrinos
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• First spectrum gt 1 TeV
• up to 100 TeV
• matches
• lower-energy
• Frejus data

PRELIMINARY
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Point source search
Search for Point Sources
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Skyplot Amanda-II, 2000
697 events below horizon
above horizon mostly fake events
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Close by objects
Sun
Crab - Nebula
Cyg-X1
LMC
SS-433
SMC
30 kpc 90 000 ly
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Intrinsic source ? spectrum (corrected for IR
absorption)
Measured ? spectrum
AMANDA average flux limit for two
assumed spectral indices ?, compared to the
average gamma flux of Markarian 501 as observed
in 1997 by HEGRA.
AMANDA-II has reached the sensitivity needed
to search from neutrino fluxes from TeV gamma
sources of similar strength to the instrinsic
gamma flux.
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Year 2000-2002 unbinned statistical analysis use
point resolution function for each individual
event

• No significant excess beyond
• expected randomly fluctuations

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For comparison the same events scrambled in
azimuth (expect no point excesses by definition)
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... and the original event sample with only the gt
3 sigma excess marked
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Expected sensitivity for AMANDA 97-03
m ? cm-2 s-1
southern sky
northern sky
4 years Super-Kamiokande
170 days AMANDA-B10
10-14
230 days AMANDA-II
8 years MACRO
10-15
declination (degrees)
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Diffuse Flux
Search for a diffuse flux of H.E.
extraterrestrial neutrinos
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Bounds and Predictions
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Experimental Limits
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Upper Limit from Energy Spectrum recorded
neutrino events
Energy spectrum in detector
How much E-2 cosmic ? signal allowed
within uncertainty?
PRELIMINARY
determine statistics in last bin with MC ?
confidence belts (FC)
E2??µ(E) lt 2.6107 GeV cm-2 s-1 sr-1
Limit on diffuse E-2 ?µ flux
Includes 33 systematic uncertainty
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... look also to cascades from electronand tau
neutrino interactions
Assuming ?e???? 120 at source ?e????
111 at Earth
factor 3 applied to ?? channel
AMANDA-II cascades
AMANDA-II ?? x 3
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Search for neutrinos correlated with Gamma Ray
Bursts
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Correlations to BATSE Gamma Ray Bursts ?
1969
BATSE 1991- May 2000
1997
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-1 hour
1 hour
10 min
Blinded Window
Background determined on-source/off-time
Background determined on-source/off-time
Time of GRB (Start of T90 )
Low background analysis due to space and time
coincidence! ? Muon effective area (averaged over
zenith angle) ? 50,000 m2 _at_ PeV
PRELIMINARY
BT BATSE Triggered BNT BATSE
Non-Triggered New IPN GUSBAD
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97-00 Flux Limit at Earth E2F? 410-8 GeV
cm-2 s-1 sr-1 (for 312 bursts with
Waxman/Bahcall Spectrum)
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• Low background (due narrow time and space
  coincidence)
• - Large effective areas (50 000 m² _at_ 1 PeV)

Upper limit 16 Waxman/Bahcall flux
with 3 years of data (1997,1999,2000)
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Indirect Search for Dark Matter
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Indirect Search for WIMPs
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(a) Neutrinos from the Center of Earth
? ?
? b b
soft spectrum
?
? W W -
hard spectrum
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Upper limits on muon flux from neutralino
annihilations in center of Earth
Green dots Excluded by present direct
searches Blue crosses can be excluded by 10
times more sensitive direct searches
Baikal 98/99 data
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Indirect Search for WIMPs
(b) Neutrinos from the Sun
?
?
?
Amanda
At South Pole the Sun sinks maximally 23 below
horizon. Therefore only Amanda-II with its
dramatically improved reconstruction capabilities
for horizontial tracks (compared to Amanda-B10)
can be used for solar WIMP search.
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Upper limits on muon flux from neutralino
annihilations in center of Sun
AMANDA-II results based on 193 days of
live time
ANTARES and ICECUBE MC-calculated sensitivities
preliminary
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Relativistic Magnetic Monopoles
10-14
Baikal 199619981999 Amanda 1997
Soudan
KGF
Baikal
10-15
MACRO
Cherenkov-Light ? n2(g/e)2
Orito
upper limit (cm-2 s-1 sr-1)
10-16
Amanda
n 1.33 (g/e) 137/ 2
? electrons
10-17
IceCube
10-18
? 8300
1.00
0.75
0.50
? v/c
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Supernova Monitor
Amanda-II
B10 60 of Galaxy A-II 95 of Galaxy
IceCube up to LMC
Amanda-B10
IceCube
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IceCube
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IceCube Collaboration

• Institutions 11 US, 10
  European, 1 Japanese and 1 Venezuelan
• Bartol Research Institute, University of Delaware
  
• BUGH Wuppertal, Germany
• Universite Libre de Bruxelles, Brussels, Belgium
• CTSPS, Clark-Atlanta University, Atlanta, USA
• DESY-Zeuthen, Zeuthen, Germany
• Institute for Advanced Study, Princeton, USA
• Lawrence Berkeley National Laboratory, Berkeley,
  USA
• Department of Physics, Southern University and
  A\M College, Baton Rouge, LA, USA
• Dept. of Physics, UC Berkeley, USA
• Institute of Physics, University of Mainz, Mainz,
  Germany
• University of Mons-Hainaut, Mons, Belgium
• Dept. of Physics and Astronomy, University of
  Pennsylvania, Philadelphia, USA
• Dept. of Astronomy, Dept. of Physics, SSEC,
  University of Wisconsin, Madison, USA
• Physics Department, University of Wisconsin,
  River Falls, USA
• Division of High Energy Physics, Uppsala
  University, Uppsala, Sweden
• Dept. of Physics, Stockholm University,
  Stockholm, Sweden
• Dept. of Physics, University of Alabama, USA

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IceCube

• - 80 Strings
• - 4800 PMT
• Instrumentiertes Volumen 1 km3
• Installation
• 2004-2010

80.000 atm.? per year
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Simulated IceCube ?? Events
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Angres
Angular resolution as a function of zenith angle
Waveform information not used. Will
improve resolution for high energies !
0.8 0.6

• above 1 TeV, resolution 0.6 - 0.8 degrees for
  most zenith angles

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IceCube Eff Area
IceCube Effective Area
Aeff / km2
cos ?
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HV Base
Flasher Board
DOM Mainboard
Delay Board
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Supernova Monitor
Amanda-II
B10 60 der Galaxis A-II 95 der Galaxis
IceCube bis zu LMC
Amanda-B10
IceCube
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Schedule and Cost
03-04 drill equipment to Pole 04-05 first
strings (proof that 16/season are feasible,
prepare 10 full strings)
05-06 16 strings 06-07 16 strings 07-08 16
strings 08-09 16 strings 09-10 remaining
strings
Overall cost with personnel, contingency,
overhead 250 M Detector 55 M
Logistics, including drilling 40 M
68
m ? cm-2 s-1
Expected sensitivities to steady point sources
10-14
2001
10-15
2003
GX 339-4
2007
10-16
typical predictions for AGN, SNR, ...
10-17
2012
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Success not guarantied, but history is on our
side
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