cosmic photons associated with cosmic rays

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cosmic photons associated with cosmic rays
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gtgtgt 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 gtgtgt
energy in cosmic rays equal to the
energy in light !
1 TeV 1.6 erg
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Neutrino Beams Heaven Earth
NEUTRINO BEAMS HEAVEN EARTH
Black Hole
Radiation Enveloping Black Hole
p g -gt n p cosmic ray neutrino
-gt p p0 cosmic ray gamma
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Neutrinos Associated With the Source of the
Cosmic Rays?
neutrino flux
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Image analysis using Hillas parameters
Proton shower ( wide, points anywhere )
alpha
Direction of primary ? - ray
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High-energy gamma-rays
TeV gamma ray astronomy

• a cosmic photon
• initiates an
• electromagnetic
• shower high in
• the atmosphere
• the shower
• particles emit
• Cherenkov
• radiation
• this radiation is
• captured by
• mirrors read out
• by a cluster of
• photomultipliers

Effective area 104m2
?8 km
Cherenkov light
?120 m
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MAGIC A next step
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HESS RX J1713 Spectrum
18 h 2003 data

• 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

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RX J1713 Spectrum

• In favor of p0
• no cut-off in the
• HE tail of HESS
• spectrum
• signal from the
• direction of
• molecular clouds

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Supernova Beam Dump
RX J1713-3946
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Neutrino Beams Heaven Earth
g n
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g-rays from p0 decay discovered ?

• ? En Nn (En) ? ? Eg Ng (Eg)

1 lt ? lt
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accelerator beam dump (hidden source)
transparent source p0 p p-
n flux predicted observed g-ray
flux 20 per km2 RX J1713-3946
per year (galactic
center)
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TeV B L A Z A R 1ES 1959650 a
posteriori coincidence
H. Krawczynski et al, 2004ApJ,601 151K
Multiwavelength Observations of Strong Flares
from the TeV Blazar 1ES 1959650
TeV Flux (Crab)
10 keV Flux (keV-1 cm-2 s-1)
orphan flare
PRELIMINARY
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Sensitivity of Gamma ray telescopes
Sensitivity to neutrinos
8 9 10 11 12
13 14 15 16
log(E/eV)
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cosmic neutrinos associated with cosmic rays
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Requires Kilometer-Scale Neutrino Detectors
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detector
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Neutrino Detection Probability
neutrino detected
neutrino survives
L _ ln
1 - e-

L
L _ ln
e-

L _ ln
_
ne
m
t
Pdet nL sn
nm
nt
for nm L Rm Em (1 - y) En for nt
L c tt
Et __ mt
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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
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the earth as a cosmic ray muon filter
l
n
Psurvival exp -(l/ ln) ln-1 n sn (En)
a neutrino of 70 TeV has an interaction length
equal to the diameter of the earth
n r NA
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detection method
lattice of light sensors
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Photomultiplier Tube
1 cm
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ANTARES Layout
ANTARES
14.5 m
350 m
Junction box
100 m
40 km to shore
60-75 m
Readout cables
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Northern hemisphere detectors
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North
AMANDA
South Pole
Dome
1500 m
Amundsen-Scott South Pole station
2000 m
not to scale
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AMANDA II
t i me

• up-going muon
• 61 modules hit

gt 7 neutrinos/day on-line
Size Number of Photons
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IceCube optical sensor
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AMANDA Event SignatureMuon
CC muon neutrino interaction ? track
nm N ? m X
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Skyplot Amanda-II, 2000
697 events below horizon
above horizon mostly fake events
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1968 OSO-3 (Kraushaar et al. 1972)
sources seen in next mission! SAS-2 100 cm2

• effective area 4 cm2
• 600 photons

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AMANDA skyplot 2000-2003 optimized for best
sensitivity to E-3 E-2 sources
3369 events below horizon
Preliminary
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n telescope point source search
Preliminary

• Search for clustering in northern hemisphere
• compare significance of local fluctuation to
• atmospheric n expectations
• un-binned statistical analysis
• no significant excess

2000-2003 (807 days) 3329 n from northern
hemisphere 3438 n expected from atmosphere
? also search for neutrinos from unresolved
sources
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2000-03 scrambled (top) and unblinded (bottom)
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Cas A
Mk501
Mk421
Cyg
Crab
M87
SS433
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Preliminary
Triangles event times
Yellow bars width of sliding search window
A posteriori 3 (of 5) events in 66 days Period
of major outburst measured at different
wavelengths in 2002 (and an orphan flare)
Error bars off-source background per 40 days
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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
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Unique observation of a high flux g-rays flare
without corresponding X-ray counterpart
Results from the multi-wavelength campaign (a)
Whipple and HEGRA (b-c) X-ray (d-f)
optical (g-h) radio ApJ 601, 151 (2004)
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Neutrinos Associated With the Source of the
Cosmic Rays?
neutrino flux
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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 (2000-2003) sensitivity

preliminary!
limits multiplied by 3 for oscillations!
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required sensitivity
... for discovering extraterrestrial neutrinos
many specific models for non-resolved sources ...
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atmospheric
E-2 flux
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? Waxman, Bahcall (1999) derive generic limits
from ? limits on extragalactic ps ? ?-ray flux
log E?2 flux(E??) / GeV cm-2 s-1 sr-1
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GZK
WB bound
AGN core (SS)
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AGN Jet (MPR)
GRB (WB)
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log (E? /GeV)
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4
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5
8
10
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6
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TeV PeV
EeV