we built a km 3 neutrino detector 3 challenges: drilling optics of ice atmospheric muons
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Transcript of we built a km 3 neutrino detector 3 challenges: drilling optics of ice atmospheric muons
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• we built a km3 neutrino detector 3 challenges:
• drilling• optics of ice• atmospheric muons
• atmospheric neutrino spectrum
• atmospheric muon spectrum: first surprise
• search for the sources of the Galactic cosmic rays
• search for the extragalactic cosmic rays
• gamma ray bursts• GZK neutrinos• a multi-wavelength story
• search for dark matter
IceCube.wisc.edu
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• Direct detection• Indirect detection:
– neutrinos from the Earth/Sun– antiprotons from the galactic halo– positrons from the galactic halo– gamma rays from the galactic halo– gamma rays from external galaxies/halos– synchrotron radiation from the galactic center /
galaxy clusters– ...
WIMP search strategies
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• Search for an annual modulation due to the Earth’s motion around the Sun
direct detection - general principles
• WIMP + nucleus WIMP + nucleus
• Measure the nuclear recoil energy
• Suppress backgrounds
December June
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present limits
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DAMA result (> 8 sigma)
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neutralino capture and annihilation
sun
Freese, ’86; Krauss, Srednicki &Wilczek, ’86 Gaisser, Steigman & Tilav, ’86
velocitydistribution
scatt
capture
annihilation
interactions
int. int.
cc ,bb ,tt , ,W, Z 0, HH 0
ll
W, Z,HSilk, Olive and Srednicki, ’85Gaisser, Steigman & Tilav, ’86
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supersymmetry onthe back of an
envelopearXiv 9404252
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WIMP Capture and Annihilation
DETECTOR
n
+ W + W +
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indirect detection for cyclists
e.g. -telescope searches for 500 GeV WIMP
> LHC limit1. - flux300 km/s
2. solar cross section
124 ]500
[104.2 scmm
GeVv
343 ]500
[1084.0 cmm
GeVcmGeV
]10][102.1[ 24157 cm
m
Mn p
p
sunpsun
2Z
2F
m
M22pF
M
G~
)mG( 4H
2Z
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Nsun = capture rate = annihilation rate
250 GeV
3. Capture rate by the sun
4. Number of muon-neutrinos
120sunsun s10x3N
sunN1.0x2N
0.1 is the leptonic branching ratio
WW500 GeV
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# events = 60 per year
1282 scm10x2
d4N
timerunningGeVEAevents 250#
2210 cm
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update: focus region
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neutrino rate versus WIMP masswhite line: 100 events km-2 yr-1
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IC22
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solar neutrino ratevs wimp mass0—1 TeV
100 events km-2 yr-1
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• capture
• equilibrium capannann
anncap
CNC
NCCdt
dN
2
1
2
1 2
2
neutrino flux
wimp-nucleon crosssection
indirect detectionindirect detectionof of
dark matterdark matter
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atm
osph
eric
neu
trin
o ev
ents
the sun
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sensitivity to wimps withspin-independent interactions
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arXiv:0906.1615
<103 SI limit
>103 SI limit
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arXiv:0906.1615
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neutrinos from thecenter of the
Galaxy
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conclusions
• supersymmetry comes in 2 flavors: spin-independent ( favors direct detection because of A2 ) and spin-dependent
• IceCube is competitive for spin-dependent
• can probe most of the interesting parameter space of the MSSM
• [astrophysics is known ( no toothfairies )]
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IceCube: multiwavelength analysis
• IceCube
• supernova explosions (millisecond alert)
• a story from AMANDA days
• TeV gamma ray observations
• GRB
IceCube takes data continuouslyand records and archives them
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supernova burst: light from
PMT noise low (280 Hz)
detect correlated rate increase on top of PMT noise when supernova neutrinos pass through the detector
enpe
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Simulation DataLuminosities
Kitaura, Janka, Hillebrandt (Astron. Astrophys. 450 (2006) 345)
Garching
first 20 msec
deleptonization
enpe
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• equivalent detection volume of a 2.5 megaton SuperK-style detector
• 1 million events from 10 kpc
• time of neutronization to a few milliseconds
starting points of neutrino showers
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CLatmsstart
samplingmwithevents
%953:
sec7.1106
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signal depends on• properties of the supernova collapse• unknown neutrino physics
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Kamioka II1987A
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Participation in SNEWS
coincidenceserver @ BNL
Super-K
alertSNO
LVD
AMANDA(IceCube)
http://snews.bnl.gov astro-ph/0406214
IceCube will follow this year
…several hours advanced notice to astronomers …