the highest energy neutrinos

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the highest energy neutrinos
francis halzen
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the neutrino view of ? extragalactic
sources ? galactic sources ? the GZK
feature
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energy (eV)
/ / / / / / / / / / / / / / / / /
n
CMB
Radio
Visible
TeV sources!
flux
cosmic rays
GeV g-rays
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Background Energy Distribution
Intensity nW m-2 sr-1
Frequency Hz
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Natures Accelerators ?
protons gt 108 TeV photons gt 102
TeV neutrinos gt 102 TeV
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extragalactic cosmic raysenergy density 3 x
10-19 erg/cm3
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galactic and extragalactic cosmic rays
1 event km -2 yr -1
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? 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
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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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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 photons neutrinos
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flux of extra-galactic cosmic rays
ankle ? one 1019 eV particle per km squared per
year per sr
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diffuse muon neutrino flux

MPR bound
100 - 500 events per km2 year
WB
HBL blazars
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active galaxy
radiation field ask astronomers

• energy in protons
• energy in electrons
• photon target observed
• in lines
• gtgt neutrino flux calculable

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0 seconds fireball protons and photons interact
PeV
EeV
TeV
- 10 seconds fireball protons interact with
remnant of the star
afterwards afterglow protons interact with
inter-stellar medium
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heavenly beam dump
e only ?
synchrotron radiation
e
?
?e
?
p
?
e-
??
n
?sync
?sync
cosmic rays exist !
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galactic cosmic raysenergy density 10-12
erg/cm3
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Cas A supernova remnant in X-rays
Shock fronts
Fermi acceleration when particles cross high
B-fields
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key issue magnetic field
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HESS RX J1713 Spectrum
18 h 2003 data
1 10 neutrinos per km2 year KM3NeT
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supernova beam dump
RX J1713-3946
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hadronic electromagnetic 4 - 4
RX J1713 on astro-ph
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? the accelerator
TeV photons trace the density of the molecular
clouds
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galactic plane
Southern Hemisphere Sky
Standard Deviations
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cygnus region Milagro and Tibet
Milagro contours are pion model with no sources
crosses are EGRET unidentified
sources TeV/matter correlation good chance
noncorrelation 1.5x10-6
24 neutrinos in IceCube per source
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????? flux of galactic cosmic rays
a SNR at d 1 kpc transfers W 1050 erg to
cosmic rays interacting with molecular
clouds with density n 1 cm-3
2 SN per century supply the observed density of
galactic cosmic rays
e.g. RX J1713.7-3946
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p-
p
p0
neutral pions are observed as gamma
rays charged pions are observed as
neutrinos nm g / 2
n m
n m-
g
g
e e-
e
g
e-
m
e
g
n
e
n
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1000 models same n-rate
egret
milagro
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cosmic neutrinos how ?
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shielded and optically transparent medium
Cherenkov radiation
array of optical sensors
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• nanosecond timing allows
• likelihood reconstruction of the
• track with degree accuracy

m
n

• photon counts reflect energy of the muon
• that loses energy catastrophically
  (bremsstrahlung,)

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antares
antares
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antares zenith angle distribution
preliminary, see talk by Antoine Kouchner
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Skyplot AMANDA and Baikal
AMANDA2000-2003, Baikal 1998-2002 galactic
coordinates
nm N ? m X
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skyplot AMANDA
AMANDA sykplot 2000-2003 3329 events below
horizon 04 ? 4282 05 and 06 done
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IceCube/IceTop

• IceTop
• 80 Stations à 2 Ice-C-Tanks
• Last year 16 stations
• 2830 m altitude
• 125 m spacing
• 3 ? 1014 lt E lt 1018 eV
• Atot 1 km2
• Last year 0.13 km²

electromagnetic

• IceCube Strings
• 4800 DOMs
• Muon bundle detector
• Emuon gt TeV

1450 m
muons
2450 m
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IceTop PeV to EeV
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IceTop-IceCube coincident event
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22 strings 1320 digital modules 52 surface
detectors
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IceCube event 22 strings
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IceCube integrated volume
cumulative km3yr of exposure volume
5
4
3
2
also NESTOR NEMO
1
2005 2006 2007 2008 2009 2010 2011 2012
2013 2014 year
? 1 km3yr reached 2 years before detector is
completed ? close to 4 km3yr at the beginning of
2nd year of full array operation
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Parameters of neutrino telescopes

• Effective ? area
• 0.1 m² _at_ 10 TeV
• 1-4 m² _at_ 100 TeV
• 30 m² _at_ 100 TeV
• 100 m² _at_ 100 TeV

AMANDA, ANTARES now IceCube complete

• Point source sensitivity
• AMANDA, ANTARES 10-10 ? / (cm² s) above 1 TeV
• IceCube 10-12 ? / (cm²
  s) above 1 TeV

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effective telescope area at 100 TeV

• AMANDA ANTARES (1- 5) m2
• IceCube 22 strings (now) 30 m2
• IceCube 80 strings (final) 100 m2

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IceCube

• in the next 10 years IceCube will observe
• 106 atmospheric neutrinos with energies
• 0.11,000 TeV
• 10 GZK neutrinos with energy gt 106 TeV
• with m0.01 eV and E100 TeV
• the gamma factor of the neutrino is

25 m
45 m
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Livingston plot energy versus year

• 1 event per year
• in IceCube
• radio/acoustic domain
• priority determine
• the event rate!

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neutrinos from GZK interactions
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cosmic rays interact with the microwave background
cosmic rays disappear, neutrinos appear
1 event per kilometer squared per year
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neutrinosfromGZKinteractions
galactic
extragalactic
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neutrino cross-section at 1018 eV ?
order of magnitude at 1020 eV
better than factor 2 at 1016 eV
flux itself is ambiguous because of spectrum and
evolution of the unknown sources
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novel detection methodsradio, acoustic and
horizontal showers
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neutrino showers
(distinguishable if almost horizontal)
downgoing (direct n interaction in atmosphere)
upgoing (n t in earth t decay in flight )
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Muons
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radio emission from neutrino-induced
electromagnetic cascades

• Electromagnetic cascades electron-positron
  pairs and
• (mostly) gammas ? electrically neutral, no
  radio emission.
• But, Compton scattering of photons on atomic
  electrons creates
• negative charge excess of 20
• Negative charge radiates coherently at MHz GHz
  ?
• Power Energy 2
• Askarian effect demonstrated at SLAC consistent
  with
• calculations

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SLAC T486 (Jul06) Askaryan on ice

• Opportunity to test the effect in a
• medium relevant to several current
• and future experiments
• ANITA, RICE, etc.

• 12-tons of ice ANITA
• End Station A SLAC beam Ideal ANITA
• calibration comprehensive
• validation of Askaryan

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current UHE neutrino limits projections

• RICE
• limits for 3500 hours livetime
• GLUE
• limits 120 hours livetime
• FORTE
• limits on 3.8 days of livetime
• ANITA-lite 18.4 days of data, net 40 livetime
  with 60 analysis efficiency for detection
• ANITA projected sensitivity
• 1.5-2.5 orders of magnitude gain!

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Existing Neutrino Limits and Future Sensitivity

• RICE limits for 3500 hours livetime
• GLUE limits 120 hours livetime
• ANITA sensitivity, 45 days total
• 5 to 30 GZK neutrinos
• IceCube high energy cascades
• 1.5-3 GZK events in 3 years
• Auger tau neutrino decay events
• 1 GZK event per year?

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RICERadio Detection in South Pole Ice
Neutrino enters ice

• Installed 15 antennas
• few hundred m depth with
• AMANDA strings.
• Tests and data since 1996.
• Most events due to local
• radio noise, few candidates.
• Continuing to take data,
• and first limits prepared.
• Proposal to Piggyback with
• ICECUBE

Neutrino interacts
Antenna Cable
Cube is .6 km on side
Two cones show 3 dB signal strength
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in-ice view of radio detection
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ANITA
Antarctic Impulsive Transient Antenna Experiment
searching for GZK neutrinos with radio detection
in Antarctic ice
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possible IceCube extensions
optical-radio-acoustic detector
IceCube Collaboration, ICRC2005
instrumented volume (110 3) km3
Optical 80 IceCube 13 IceCube-Plus strings
at a 1 km radius, 1.5-2.5 km depth Radio/Acousti
c 91 holes, 1 km spacing, 1.5 km depth 5 radio
300 acoustic receivers per hole
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EVENT RATES
IceCube CoIlaboration, ICRC2005
Detection option GZK events/year)
IceCube 0.7
Optical 1.2
Radio 12.3
Acoustic 16.0
OpticalRadio 0.2
OpticalAcoustic 0.3
RadioAcoustic 8.0 !!!
Opt.Rad.Acou. 0.1
TOTAL 21.1
Numbers calculated, folding effective volumes
with ESS GZK neutrino flux model
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staged IceCube enhancements
Optical 80 IceCube 13 IceCube-Plus
(astro-ph/0310152) holes at 1 km radius (2.5 km
deep) Radio/Acoustic determine GZK event rates
with 6 12 radio detectors at the surface or at
depth calibration with IceCube!
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ARIANNA concept100 x 100 station array, 1/2
Teraton
Ross Ice Shelf, Antarctica
300m
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reflected and direct events
n
n
ice
ignore
Direct
Reflected (much greater solid angle)
sensitivity to neutrino cross section
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The Thermo-Acoustic Model
G.A. Askaryan, At. Energ., vol.3, no.8, (1957)
p.152 Askaryan, Dolgoshein, Kalinovsky, NIM
164(1979) 267
? vol. expans. coefficient Cp specific
heat
? Particle cascades produce pressure pulses?
Pressure amplitude measures incoming energy ?
Pressure distribution measures incoming
direction? Frequency 10-100 kHz
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TODAY ACTIVITIES AT MANY SITES
group experiment activities
Stanford SAUND data taking, signal processing, calibration , simulation
INR1 AGAM, MP10 signal processing, calibration , simulation
INR2, Irkutsk Baikal signal processing, noise studies, in-situ tests at Baikal
ITEP Baikal,Antares detector RD, accel. tests, in-situ tests at Baikal, signal proc., noise st.
Marseille Antares detector and installation RD, calibration, noise studies, simulation,
Erlangen Antares, KM3NET detector RD, accel. tests, calibration, simulation, noise studies, in-situ test measurements
Italy KM3NET detector RD
Italy NEMO installation RD, noise studies, simulation
UK Rona, KM3NET simulation, signal processing , calibration
US Salt Dome detector RD, attenuation studies, material studies
Aachen IceCube detector RD, general purpose ice test laboratory
IceCube detector RD, accel. tests, material studies, simulation, noise studies, in- situ test measurements (SPATS)

ARENA 2005 http//www-zeuthen.
desy.de/arena
ARENA 2006 http//www.shef.ac.uk
/physics/arena
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2005, 2006, 2007 deployments
AMANDA
a km squared year data by 0809
IceCube string and IceTop station deployed 01/05
IceCube string and IceTop station deployed 12/05
01/06
data from completed Antares detector ? KM3NET
IceTop station only 2006
IceCube string and IceTop station to be deployed
12/06 01/07
new ANITA flight in summer 08-09

• 604 DOMs deployed to date
• Want to achieve steady state of 14 strings /
  season.