Transcript cosmic photons associated with cosmic rays >>> energy in extra-galactic cosmic rays: ~ 3x10-19 erg/cm3 or ~ 1044 erg/yr per (Mpc)3 for 1010

cosmic photons associated with
cosmic rays
>>> energy in extra-galactic cosmic rays:
~ 3x10-19 erg/cm3 or
~ 1044 erg/yr per (Mpc)3 for 1010 years
3x1039 erg/s per galaxy
3x1044 erg/s per active galaxy
2x1052 erg per gamma ray burst
>>> energy in cosmic rays ~ equal to
the energy in light !
1 TeV = 1.6 erg
Neutrino Beams: Heaven & Earth
NEUTRINO BEAMS: HEAVEN & EARTH
Black Hole
Radiation
Enveloping
Black Hole
p + g -> n + p+
~ cosmic ray + neutrino
-> p + p0
~ cosmic ray + gamma
Neutrinos Associated With the Source of the Cosmic Rays?
neutrino flux
AMANDA II
sensitivity(!)
•a cosmic photon
initiates an
electromagnetic
shower high in
the atmosphere
High-energy
TeV
gamma ray gamma-rays
astronomy
Effective area:
104m2
•the shower
particles emit
Cherenkov
radiation
•this radiation is
captured by
mirrors read out
by a cluster of
photomultipliers
8 km
120 m
MAGIC – A next step
HESS: RX J1713 Spectrum
• first resolved
image of
supernova
remnant
in TeV photons
• (theoretical)
evidence for
the acceleration
of protons at
the level
required to
explain
galactic cosmic
rays
18 h 2003 data
RX J1713 Spectrum
H.E.S.S.: full remnant
CANGAROO: hotspot
Index 2.2±0.07±0.1
Index
2.84±0.15±0.20
preliminary
In favor of p0:
• no cut-off in the
HE tail of HESS
spectrum
• signal from the
direction of
molecular clouds
Supernova
Beam
Dump
RX J1713-3946
Neutrino Beams: Heaven & Earth
gn
g-rays from p0 decay discovered ?
En Nn (En) =  ∫ Eg Ng (Eg)
transparent
source
p0 = p+ = p-
1
<<
n flux predicted
~20 per km2
per year
8
∫
accelerator
beam dump
(hidden source)
observed g-ray flux
RX J1713-3946
(galactic center)
TeV B L A Z A R 1ES 1959+650
a posteriori coincidence
TeV Flux (Crab)
10 keV Flux (keV-1 cm-2 s-1)
H. Krawczynski et al, 2004ApJ,601 151K
‘Multiwavelength Observations of Strong
Flares from the TeV Blazar 1ES
1959+650’
“orphan” flare
PRELIMINARY
Sensitivity of
Gamma ray telescopes
Sensitivity to neutrinos
AMANDA (neutrinos)
IceCube (neutrinos)
8
9
10
11
12
13
14
15
16
Sensitivity (2π sr, 100% ontime):
3 years exposure, 5 sigma
log(E/eV)
E-2
cosmic neutrinos associated with
cosmic rays
Requires
Kilometer-Scale
Neutrino
Detectors
detector
• infrequently, a cosmic neutrino is
captured in the ice, i.e. the
neutrino interacts with an
ice nucleus
• in the interaction a muon (or electron,
or tau) is produced
muon or tau
Cerenkov
light cone
interaction
•the muon radiates blue light in its wake
•optical sensors capture (and map) the light
neutrino
Neutrino Detection Probability
neutrino
detected
neutrino
survives
e
-
L
_
L
L
_
ln
ne m
t
nm nt
for nm : L
Rm [Em = (1 - y) En]
for nt : L
E
__t c t
t
mt
1
-l
-e n
L
~
_ _
ln
Pdet= nL sn
Detection of n(En)
Nevents = Psurvival Pdetected Area n
Area = L2
for detailed geometry and kinematics:
Physics Reports 258 (3), 173 (1995)
hep-ph/0105067
the earth as a
cosmic ray muon filter
l
n
a neutrino of 70 TeV has an
interaction length equal to the
diameter of the earth
Psurvival = exp -(l/ ln)
ln-1 = n sn (En)
n = r NA
detection method
lattice of light sensors
Photomultiplier Tube
1 cm
ANTARES
ANTARES Layout
14.5 m
350 m
100 m
Junction
box
40 km to
shore
~60-75 m
Readout cables
Northern hemisphere detectors
Baikal NT200
1100 m deep
data taking since 1998
new: 3 distant strings
Antares
March 17, 2003
2 strings connected
2400 m deep
completion: start 2006
Nestor
March 29, 2003
1 of 12 floors deployed
4000 m deep
completion: 2006
“North”
AMANDA
South Pole
Dome
1500 m
2000 m
[not to scale]
Amundsen-Scott South Pole station
AMANDA II
• up-going muon
t
i
m
e
• 61 modules hit
> 7 neutrinos/day
on-line
Size ~Number of
Photons
IceCube optical sensor
AMANDA Event
Signature:
Muon
CC muon neutrino
interaction
 track
nm + N  m + X
Skyplot Amanda-II, 2000
697 events
below horizon
above horizon:
mostly fake events
1968 OSO-3 (Kraushaar et al. 1972)
• effective area 4 cm2
• 600 photons
sources seen in
next mission!
SAS-2 100 cm2
AMANDA skyplot 2000-2003
optimized for best sensitivity to E-3 – E-2 sources
3369 events
below horizon

n telescope : point source search
Maximum significance 3.4 s
compatible with atmospheric n
Preliminary
2000-2003 (807 days)
3329 n from northern hemisphere
3438 n expected from atmosphere
Search for clustering in northern hemisphere
• compare significance of local fluctuation to
~92%
atmospheric n expectations
• un-binned statistical analysis
• no significant excess
2000-03: scrambled (top) and unblinded (bottom)
Cas A
Mk421
Mk501
Cyg
Crab
M87
SS433
Yellow bars:
width of sliding
search window
Error bars:
off-source
background
per 40 days
Triangles:
event times
“A posteriori”:
3 (of 5) events in 66 days
Period of major outburst
measured at different
wavelengths in 2002
(and an “orphan flare”)
Red lines:
AMANDA – 2.25o search bin
“Orphan flare”
(MJD 52429)
Probability of a random coincidence
with the “orphan flare” or the enhanced g-ray activity undefined: a-posteriori
hypothesis relative to the test
Unique observation
of a high flux g-rays
flare without
corresponding X-ray
counterpart
Results from the multiwavelength
campaign
(a) Whipple and
HEGRA
(b-c) X-ray
(d-f) optical
(g-h) radio
ApJ 601, 151 (2004)
Neutrinos Associated With the Source of the Cosmic Rays?
neutrino flux
AMANDA II
sensitivity(!)
diffuse neutrino flux limits 2005
1.MACRO
2.AMANDA B10 nm (1997)
3. AMANDA-B10 UHE (1997)
4. AMANDA-II cascades (2000)
5. Baikal cascades 1998-2003
6. AMANDA-II nm-analysis (2000)
7.AMANDA-II UHE sensitivity !!
8. AMANDA nm-analysis (20002003) sensitivity
preliminary!
limits multiplied by 3
for oscillations!
required sensitivity
log [En2 · flux(En) / GeV cm-2 s-1 sr-1]
... for discovering extraterrestrial neutrinos
many specific models for
non-resolved sources ...
-5
E-2 flux
-6
 Waxman, Bahcall (1999)
-7
derive generic limits from
 limits on extragalactic p‘s
 g-ray flux
WB bound
GZK
-8
-9
2
GRB (WB)
3
TeV
4
5
6
PeV
7
8
9
EeV
10 log (En /GeV)