• 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

• 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

• 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

present limits

DAMA result (> 8 sigma)

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

qq

ll

W, Z,HSilk, Olive and Srednicki, ’85Gaisser, Steigman & Tilav, ’86

supersymmetry onthe back of an

envelopearXiv 9404252

WIMP Capture and Annihilation

DETECTOR

n

+ W + W +

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

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

# events = 60 per year

1282 scm10x2

d4N

timerunningGeVEAevents 250#

2210 cm

update: focus region

neutrino rate versus WIMP masswhite line: 100 events km-2 yr-1

IC22

solar neutrino ratevs wimp mass0—1 TeV

100 events km-2 yr-1

• 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

atm

osph

eric

neu

trin

o ev

ents

the sun

sensitivity to wimps withspin-independent interactions

arXiv:0906.1615

<103 SI limit

>103 SI limit

arXiv:0906.1615

neutrinos from thecenter of the

Galaxy

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 )]

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

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

Simulation DataLuminosities

Kitaura, Janka, Hillebrandt (Astron. Astrophys. 450 (2006) 345)

Garching

first 20 msec

deleptonization

enpe

• 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

CLatmsstart

samplingmwithevents

%953:

sec7.1106

signal depends on• properties of the supernova collapse• unknown neutrino physics

Kamioka II1987A

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 …