Neutrino Astronomy Neutrino Astronomy at the South Poleat the South Pole
David BoersmaDavid BoersmaUW MadisonUW Madison
Lake Louise Winter InstituteLake Louise Winter InstituteChicago, 23 February 2006Chicago, 23 February 2006
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IceCube CollaborationIceCube Collaboration
• Universität Wuppertal, Germany• MPI Heidelberg• Uppsala university, Sweden• Stockholm university, Sweden• Imperial College, London, UK• Oxford university, UK• Utrecht University, Netherlands
• Universität Wuppertal, Germany• MPI Heidelberg• Uppsala university, Sweden• Stockholm university, Sweden• Imperial College, London, UK• Oxford university, UK• Utrecht University, Netherlands
• Universite Libre de Bruxelles, Belgium• Vrije Universiteit Brussel, Belgium• Université de Gent, Belgium • Université de Mons-Hainaut, Belgium• Universität Mainz, Germany• Humboldt Universität, Germany• DESY-Zeuthen, Germany• Universität Dortmund, Germany
• Universite Libre de Bruxelles, Belgium• Vrije Universiteit Brussel, Belgium• Université de Gent, Belgium • Université de Mons-Hainaut, Belgium• Universität Mainz, Germany• Humboldt Universität, Germany• DESY-Zeuthen, Germany• Universität Dortmund, Germany
• Alabama University, USA• University of Alaska, Anchorage, USA• Bartol Research Institute, Delaware, USA• Pennsylvania State University, USA• UC Berkeley, USA• UC Irvine, USA• Clark-Atlanta University, USA• University of Maryland, USA• IAS, Princeton, USA• University of Wisconsin, Madison, USA• University of Wisconsin, River Falls, USA• LBNL, Berkeley, USA• University of Kansas, USA• Southern University and A&M College, Baton Rouge, USA
• Alabama University, USA• University of Alaska, Anchorage, USA• Bartol Research Institute, Delaware, USA• Pennsylvania State University, USA• UC Berkeley, USA• UC Irvine, USA• Clark-Atlanta University, USA• University of Maryland, USA• IAS, Princeton, USA• University of Wisconsin, Madison, USA• University of Wisconsin, River Falls, USA• LBNL, Berkeley, USA• University of Kansas, USA• Southern University and A&M College, Baton Rouge, USA
USA (14)USA (14)Europe (15)Europe (15) JapanJapan
New ZealandNew ZealandANTARCTICA
• Chiba University, Japan• University of Canterbury, Christchurch, New Zealand
• Chiba University, Japan• University of Canterbury, Christchurch, New Zealand
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Amundsen-Amundsen-Scott South Scott South Pole StationPole Station
Population:Austral Summer: ~240 peopleAustral Winter: ~60 people
South PoleDome
Summer camp
AMANDA
road to work
1500 m
2000 m
[not to scale]
IceCube
ANTARTICAANTARTICA
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Cosmic Ray SpectrumCosmic Ray Spectrum
?
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High Energy neutrinosHigh Energy neutrinos
Neglecting absorption (uncertain) Targets: p or ambient
Beam-dump model:0 -astronomy ± -astronomy
00
pp
ee ee
e e
Berezinsky et al, 1985Gaisser, Stanev, 1985
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Neutrino Neutrino DetectionDetection
μ
νμ
νμμ
X X’
W
Angle(νμ,μ) ≈ 1° (at E=1TeV)
Detected energy deposit by muon gives lower limit for energy of neutrino
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Neutrino Neutrino DetectionDetection
νe,τ
N X
W
e,τ
νμ,e,τ
N X
Z
νμ,e,τ
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AMANDAAMANDA
AMANDA-II (2000 – 200x)AMANDA-II (2000 – 200x)• 677 OMs on 19 strings677 OMs on 19 strings• Ø 200m, 500m tall200m, 500m tall• Trigger rate 80 HzTrigger rate 80 Hz• Since 2003: TWR Since 2003: TWR
AMANDA-B10 (1997-1999)• 302 OMs on 10 strings• Ø 120m, 500m tall• DAQ: TDC/ADC (surface)
AMANDA-A (1996)
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AMANDA research topicsAMANDA research topics Steady sources of neutrinosSteady sources of neutrinos
Point sources (e.g. AGNs)Point sources (e.g. AGNs) Diffuse flux (with muons)Diffuse flux (with muons) Diffuse flux (with cascades)Diffuse flux (with cascades) Atmosphere (cosmic rays)Atmosphere (cosmic rays) Gravitationally trapped WIMPsGravitationally trapped WIMPs
Exotics: e.g. magnetic monopolesExotics: e.g. magnetic monopoles Search for sources with time variabilitySearch for sources with time variability
GRBsGRBs Supernova explosionsSupernova explosions Flarers from e.g. AGNs, magnetarsFlarers from e.g. AGNs, magnetars
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Point source searchPoint source searchCombined data from 2000-2003 (livetime 807 days) 3329 (upward going) neutrino events Highest excess: 3.4 sigma (chance probability:
92%) Crab nebula: 10 events, <Nbg>=5.4 (chance
probability with 33 source candidates: 64%)
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Atmospheric Muons & Atmospheric Muons & NeutrinosNeutrinos
E deposited Nch
Get Eν and Eμ through unfolding
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WIMPs from the SunWIMPs from the Sun
ν
l
χ + χ → ν + ν (+…)
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Limits on muon flux from Earth center
Limits on muon flux from Sun
WIMP search in WIMP search in AMANDAAMANDA
Submitted for publication Published in Astrpart. Phys.
Disfavored by direct search (CDMS II)
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Let’s build a bigger one: IceCubeLet’s build a bigger one: IceCube
In-Ice Array:Number of strings: 80 (9)Optical Sensors: 4800 (540)Depth: 1450-2450mInstr. Volume: 0.9 km3
Angular Resolution: 0.6°
Surface Array (IceTop):
160 (32) tanks (2 per in-ice string)
2 DOMs per tank
Total 320 DOMs (64)
Construction: 2004-2010(status February 2006)
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main board
LED flasher board
PMT base
25 cm PMT33 cm Benthosphere
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High Energy muonsHigh Energy muons
Eμ = 6 PeV
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ContainedContainedHigh Energy High Energy
ShowerShower
E = 375 TeV
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High Energy TauHigh Energy Tau(double bang)(double bang)
E ≈ 10 PeV
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Ice is a quiet detection Ice is a quiet detection mediummedium
September 2005 InIce Noise Rates
0
100
200
300
400
500
600
700
800
900
1000
0 4 8 12 16 20 24 28 32 36 40 44 48 52 56 60
String 21 DOM Position
Rate
(H
z)
Phenol
Bat
Bucatini
ConchiglieSchneider
Weisse
ErikSegersaell Gnu
OxygenDubbel
Porter
Avocado
(compare: expected ~60kHz per OM in ANTARES)
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First First IceTop-IceCube IceTop-IceCube
coincidence coincidence eventevent
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Conclusions & OutlookConclusions & Outlook
AMANDA showed the feasibility of AMANDA showed the feasibility of High Energy Neutrino astronomy High Energy Neutrino astronomy with ice as the detection medium.with ice as the detection medium.
IceCube will be the coolest neutrino IceCube will be the coolest neutrino telescope on Earth.telescope on Earth.
Maybe extended with acoustic Maybe extended with acoustic detectors (extension to EHE)detectors (extension to EHE)
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Extra MaterialExtra Material
Specs AMANDA (resolution etc.)Specs AMANDA (resolution etc.) IceTopIceTopGRBGRBDeploymentDeploymentFlasherFlasher
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time recorded on OM
AMANDA-II
μ trackspointing error : 1.5º -
2.5º σ[log10(Eμ/TeV)]: 0.3 - 0.4
coverage: 2πCascades (particle showers)
pointing error: 30º - 40º σ[log10(Ec/TeV)]: 0.1 - 0.2
coverage: 4πcosmic rays (+SPASE)
combined pointing err :< 0.5º
σ[log10(Ep/TeV)]: 0.06 - 0.1Nucl. Inst. Meth. A 524, 169
(2004)energy deposited in OM
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IceTop
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27.1, 10:08: Reached maximum depth of 2517 m28.1, 7:00: preparations for string
installation start9:15: Started installation of the first DOM
22:36: last DOM installed 12 min/DOM22:48: Start drop
29.1, 1:31: String secured at depth of 2450.80 20:40: First communication to DOM
IceCube’s First String: January 28, 2005
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All 60 DOMs