icecube
DESCRIPTION
IceCube. Outlook for Neutrino Detection at the South Pole. S Robbins University of Wuppertal Moriond - “ Contents and Structures of the Universe ” La Thuile, Italy, March 2006. Scientific Goals IceCube Status AMANDA Results. Amundsen-Scott South-Pole Station. Alabama University, USA - PowerPoint PPT PresentationTRANSCRIPT
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IceCubeIceCube
S Robbins
University of Wuppertal
Moriond - “Contents and Structures of the Universe”
La Thuile, Italy, March 2006
Outlook for NeutrinoDetection at the South Pole
Outlook for NeutrinoDetection at the South Pole
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• Scientific Goals
• IceCube Status
• AMANDA Results
Amundsen-Scott South-Pole Station
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USA (14)USA (14)Europe (15)Europe (15)
JapanJapan
New ZealandNew Zealand
• Alabama University, USA• Bartol Research Institute, Delaware, USA• Pennsylvania State University, USA• UC Berkeley, USA• UC Irvine, USA• Clark-Atlanta University, USA• University of Alaska, Anchorage, USA• Univ. of Maryland, USA
• Alabama University, USA• Bartol Research Institute, Delaware, USA• Pennsylvania State University, USA• UC Berkeley, USA• UC Irvine, USA• Clark-Atlanta University, USA• University of Alaska, Anchorage, USA• Univ. 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
• 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
• Universite Libre de Bruxelles, Belgium• Vrije Universiteit Brussel, Belgium• Université de Mons-Hainaut, Belgium• Universiteit Gent, Belgium• Humboldt Universität, Germany• Universität Mainz, Germany• DESY Zeuthen, Germany• Universität Dortmund, Germany
• Universite Libre de Bruxelles, Belgium• Vrije Universiteit Brussel, Belgium• Université de Mons-Hainaut, Belgium• Universiteit Gent, Belgium• Humboldt Universität, Germany• Universität Mainz, Germany• DESY Zeuthen, Germany• Universität Dortmund, Germany
• Universität Wuppertal, Germany• MPI Heidelberg, Germany • Uppsala University, Sweden• Stockholm University, Sweden• Imperial College, London, UK• Oxford University, UK• Utrecht University, Netherlands
• Universität Wuppertal, Germany• MPI Heidelberg, Germany • Uppsala University, Sweden• Stockholm University, Sweden• Imperial College, London, UK• Oxford University, UK• Utrecht University, Netherlands
• University of Canterbury, Christchurch, NZ• University of Canterbury, Christchurch, NZ
ANTARCTICA
The IceCube Collaboration
• Chiba University, Japan• Chiba University, Japan
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Physics GoalsDetect neutrinos from the sources of cosmic-rays
Search for neutrinosfrom dark matterannihilations
Search for neutrinos from cosmological events
NewPhysics
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Fermi acceleration of protons gives particle spectrum
dNp/dE~ E-2
Neutrino production at source: p+ or p+p collisions gives pions
± -> ± +
± -> e± + + e
Neutrino flavors:
e : : 1:2:0 generic sources1:1:1 after oscillations
Observing Neutrinos
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IceCube
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IceTop air shower array80 pairs of ice Cherenkov tanks
IceCube (deep ice)80 strings of 60 optical modules17 m between optical modules125 m between strings1 km3 (1 Gton) detector!
AMANDA19 strings, 677 OMs totalø 200m, height 500m
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~1
0-20
m
Optical module
Mean - angle is ~0.7o at 1TeV
Muon travels a large distance Interaction can be outside the detector Active volume is much larger than the detector
Proposed by Markov 1960
νμμ
X X’
W
detection principle
energy deposited in OM
time recorded on OM
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Optical module
νe,τ
N X
W
e,τ
νμ,e,τ
N X
Z
νμ,e,τ
Charged-current interactions:
Neutral-current interactions:
e & detection principle
energy deposited in OM
time recorded on OM
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Ice Properties• Ice not uniform in depth (e.g. dust layers)• Important to understand ice for analysis
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Mean scattering length: 25m Mean absorption length: 110m
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Light Propagation• Cherenkov cone from muon tracks• Use timing information, accounting for propagation
Homogeneous ice Depth Dependent ice properties
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Hot-water drilling
Hose reel Drill tower
IceTop tanks5 MW Hot water generator
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AMANDA
IceCube Today
500 m
Only IceToptank
InIce string& IceTop
• 2004/2005 season– New hot water drill – First string deployed (string 21)– Four IceTop stations installed
(16 OMs)– 60 OMs in deep ice,
all 60 functioning
• 2005/2006 season– Modified drill – 8 strings deployed– 12 IceTop stations installed– 480 OMs in deep ice
and 48 OMs in IceTop
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“String 21” DataFirst IceCube string, deployed January 2005
Neutrino candidate9 string
Downgoing
IceCube event
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AMANDA
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IceTop air shower array80 pair of ice Cherenkov tanks
IceCube (deep ice)80 strings of 60 optical modules17 m between optical modules125 m between strings1 km3 (1 Gton) detector!
AMANDA19 strings, 677 OMs totalø 200m, height 500m
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“Diffuse Limits”• Measure the neutrino energy spectrum• Search for a break in the spectrum
Some AGN models excluded at 90% CL :Szabo-Protehoe 92
Stecker, Salamon. Space Sc. Rev. 75, 1996
Protehoe. ASP Conf series, 121, 1997E2μ
(E) < 2.6·10–7 GeV cm-2 sr-1 s-1
Results from one year (2000) of data
Consistent with Atmospheric neutrino expectation
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Point Source SearchNeutrino sky map:
• 2000-2003 data: 807 days livetime• 3329 neutrino events• Largest significance = 3.4 (92% chance occurrence)• No significant excess observed
• 2000-2003 data: 807 days livetime• 3329 neutrino events• Largest significance = 3.4 (92% chance occurrence)• No significant excess observed
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Neutrinos from GRBs
10 min -1 hour+1 hour
1.4501.29312 (BT)B-10/A-II97-00
1.8800.6046 (New)A-II2000
1.4701.24114 (All)A-II2000
2000
2000
1999
1998
1997
Year
A-II
A-II(2 analyses)
B-10
B-10
B-10
Detector
2.1900.2424 (BNT)
1.72/2.050/00.83/0.4044 (BT)
2.2400.2096 (BT)
2.2400.2094 (BT)
2.4100.0678 (BT)
Event U.L.NObsNBG, PredNBursts
Using space and time coincidence leads to a very low background.
No observed signal
Only ~1 order of magnitude above Waxmann&Bahcall prediction
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Solar WIMPs
• Neutralinos captured in the Sun• These annihilate producing quarks and leptons• And neutrinos, which we search for with IceCube
χ + χ → ν + ν (+…)
Earth
Detector
Freese, ’86; Krauss, Srednicki & Wilczek, ’86 Gaisser, Steigman & Tilav, ’86
Silk, Olive and Srednicki, ’85Gaisser, Steigman & Tilav, ’86
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Neutralinos from the Sun
data from 2001
Sun
Limits on muon flux from Sun
IceCube Best-Case
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Conclusions• 2005/6 was a successful deployment season• Now have in total 604 optical modules installed• Only ~1% failure rate• IceCube is on track for 1km3 neutrino observatory• AMANDA has taken 10 years of data• AMANDA continues to produce physics results
• No extraterrestrial neutrinos observed so far
• Stay tuned…