• 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