• Astroparticle Physics with High Energy Neutrinos: from AMANDA to IceCube

astro-ph/0602132

• Lectures on High Energy

Neutrino Astronomy

astro-ph/0506248

• Latest Results

astro-ph/0509330

Flux Estimates of Cosmic Neutrinos

Generic fluxes associated with cosmic rays

Astrophysics: gamma ray bursts & starbursts

Particle physics: cold dark matter search

Examples of Science

Nature’s Particle Accelerators• Electromagnetic Processes:

– Synchrotron Emission

• E~ (Ee/mec2)2 B

– Inverse Compton Scattering

• Ef ~ (Ee/mec2)2 Ei

– Bremsstrahlung

• E ~ 0.5 Ee

• Hadronic Cascades

– p + ± +o +… e ± + + +…

– p + p ± +o +… e ± + + +…

Radio Optical X-ray GeV TeV

E2 dN/dEor

F

Typical Multiwavelength Spectrum from Non-Thermal High Energy -ray Source

[ Energy

Emitted ]

[ Photon Energy ]

synchrotron

Inverse Compton

Spinning Neutron Star Fills Nebula with Energetic Electrons

Synchrotron Radiation and Inverse Compton Scattering

Active Galactic Nuclei

Massive Black Hole Accelerates Jet of Particles to Relativistic Velocities Synchrotron Emission and Inverse Compton

no evidence for protons but … cosmic rays exist

gamma ray bursts

eenp

e-

p+

R < 108 cmR 1014 cm, T 3 x 103

secondsR 1018 cm, T 3 x 1016 seconds

E 1051 – 1054 ergs

6 Hours 3 Days

Radio

Optical

-ray

X-ray (2-10 keV)

Fireball Phenomenology & The Gamma-Ray Burst (GRB) Neutrino ConnectionFireball Phenomenology & The Gamma-Ray Burst (GRB) Neutrino Connection

ProgenitorProgenitor(Massive star)(Massive star) Magnetic Field

---

Electron

-ray

collapse of massivestar produces a

gamma ray burst

spinning black hole

highest energy

particles

neutrinos from GRBneutrinos from GRB

protons and photons coexist in the fireballprotons and photons coexist in the fireball

• fireball: expanding collimated shocked jet of photons,electrons and positrons becomes optically thin

• produces neutrinos in internal collisions when slowermaterial is overtaken by faster in the fireball

NUMEROLOGYL = 1052 erg/s

R0 = 100 km (t = 10 msec)

E = 1 MeV

= 300

dE/dt = dECR/dt = 4x1044 erg Mpc-3yr-1

tH = 1010 years

Pdet = 10-6 E0.8 (in TeV)

p = 10-28 cm2 for p+n+< xp > = 0.2

GRB1 fireballfireball frameat t=0

observer frame

~ 10~ 1022 - 10 - 1033

E = E = E' E' t = t = t' t'

dd

R = c t = R0 with R0 = R' (t = 0)

RR

RRR'R'

ccvv

1 MeV10 msec

grb 2 : kinematics

R

v

c

300

cv

1

1cv

cos

km100R

2

2

0

)cv

1(c2

R)

cv

1(cR

)cosRR(c1

cd

t

2

2

EE

1c2

Rt

obs

2obs

secm101

GRB1 fireballfireball frameat t=0

observer frame

~ 10~ 1022 - 10 - 1033

E = E = E' E' t = t = -1 -1 t't'

dd

R = c t = R0 with R0 = R' (t = 0)

RR

RRR'R'

ccvv

1 MeV10 msec

GRB2GRB2Photon Density in the Fireball

nn = = = = U'U'______E'E' E'E'______

LLt/t/____________44R'R'22R'R'

R' = R' = 22cctt

R' = R' = cctt

note: for note: for = 1 (no fireball) the optical = 1 (no fireball) the optical depth of photons is depth of photons is

optopt = = R = = R00nnThTh ~ 10 ~ 101515RR00____ ThTh

GRB3pion (neutrino) production when

protons and photons coexist

p n+ neutrinos

n0 gamma rays

E'E'pp > > mm22

- m - m22pp__________________

4E'4E'Ep > 1.4 x 104 TeV

E = 1/4 < xp > Ep 1/20 Ep 700 TeV~~__ ~~__

fraction of GRB energy converted into pion (neutrino)

production

eesynchro + IC (L)

pp pions (LCR)GRB4

GRB

ppp

p

'

n1

with%15xR

f

UU______EE

cc____44

1 1 ______ EE

dEdE____dtdt

GRB 5

= = = = ((1/21/2 f f t tHH ))

charged pions onlycharged pions only

NNeventsevents = P = Psurvived survived PPdetecteddetected

20 km -2 yr -1

LLCRCR LL

~~__

~~__

Neutrino flux from GRB fireballs

cc____44

distribution of the sources critical !

Adding Fluctuations to the average:

• dN/dE: Source spectrum• f(z): redshift distribution

function, with the integral normalized to One

• E(source) = (1+z) E(here)

Num

ber

of G

RB

s

Events [km ]-2

50

45

40

35

25

30

20

15

105

010 10 10 10 10 10 10-5 -4 -3 -2 -1 0 1

(a)

fluctuations dominate !

Off source

GRB search bin

GRB Position

1 hour 1 hour16 s

BKG - off time BKG - off timeon time

GRB burst

88 BATSE bursts in 1997

background cuts can beloosened considerably high signal efficiency

effective area

~ 0.05 km2

Correlations to GRB

starbursts

starburstsstarbursts

• l ~ 100 pc

• v ~ 100 km/s

• t ~ 106 years

• ~ 0.2 g cm-2

• B ~ 0.1 mGauss

supernovae

cosmic rays

+ dense gas

pions

merging galaxies

neutrino radio connection

cosmic rays + dense gas cosmic rays + dense gas

pions electrons radiopions electrons radio

neutrinosneutrinos

starburst neutrino fluxstarburst neutrino flux

)evolutionz(5.0for

srscmGeV10

]L4[t4c

21

E

1127

H2

~ 500 eventsper km2 year

IceCube

search for dark matter particles

relic densitydecoupling occurs when

ann < H

Planck

22/1

*

T/m2/3

eq

ann

mT

g66.1)T(H

e2

Tmgn

n v

H Tf m

20

h2 3 10 27 cm3s 1

annv annv annv WIMP

1

the MSSM

The LightestSupersymmetric Particle (LSP)

Usually the neutralino. IfR-parity is conserved, it is stable.

The Neutralino –

Gaugino fraction

1. Select MSSM parameters

2. Calculate masses, etc

3. Check accelerator constraints

4. Calculate relic density

5. 0.05 < h2 < 0.5 ?

6. Calculate fluxes, rates,...

Calculation done with˜ 1

0 N11˜ B N12

˜ W 3 N13˜ H 1

0 N14˜ H 2

0

Zg N11

2 N12

2

http://www.physto.se/~edsjo/darksusy/

• 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

EdelweissJune 2002

WIMP Capture and Annihilation

DETECTOR

n

+ W + W +

indirect detection for cyclists

e.g. 101044 m m22 -telescope searches for 500 GeV WIMP

> LHC limit1. - flux300 km/s

2. solar cross section

12

Z

4 scm]mGeV500

[10x4.2v

3

Z

43 cm]mGeV500

[10x8GeVcm4.0

]cm10][10x2.1[

mM

n

24157

pp

sunpsun

2Z

2F

m

M22pF

M

G~

)mG( 4H

2Z

Nsun = capture rate = annihilation rate

_ WW

250 GeV250 GeV500 GeV

3. Capture rate by the sun

4. Number of muon-neutrinos

120sunsun s10x3N

sunN1.0x2N

is the leptonic branching ratio

5.5 x 1023 cm-3

104 m2

~~__

# events = 10 per year

1282 scm10x2

d4N

Rtimeareaevents ice

)E21

E(m625)GeV(Em5R

cm10x5.2)GeV(Ecm10 236238

Disfavored by direct search (CDMS II)

Limits on muon flux from Earth Limits on muon flux from Sun

WIMP search

PRELIMINARY

1km3 (IceCube)

AMANDA 1y

Antares 3 yearsSK

DirectDetection

(Zeppelin4/Genius)

Black: outGreen: yes

Blue: no

IceCubevs

Inner Core Detector

Inner Core(same regionas AMANDA)

7 IceCube + 18 AMANDA strings

225 DOMs + 540 OMs

7 IceCube + 18 AMANDA strings

225 DOMs + 540 OMs