Electron and Neutrino Interactions on Nucleons and Nuclei in the Next Decade
High Energy Neutrino Astronomy a promising decade ahead
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High Energy Neutrino Astronomy
a promising decade ahead
Christian Spiering, Gran Sasso, October 2002
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Content
1. Physics Goals
2. Detection Methods and Projects
3. The next decade
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1. Physics Goals A. High Energy Neutrino Astrophysics B. Particle Physics WIMPs, Magnetic Monopoles, Oscillations, Neutrino Mass ... C. Others Supernova Bursts, CR composition, Black Holes, ...
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Cosmic Rays
1 TeV
Emax ~ B LEmax ~ B L
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Supernova shocksexpanding in
interstellar medium
Crab nebula
up to 1-10 PeV
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Active Galaxies: accretion disk and jets
VLA image of Cygnus A
up to 1020 eV
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log(
E2
Flu
x)
log(E/GeV)TeV PeV EeV
3 6 9
pp core AGN p blazar jet
Top-down
GRB (W&B)
WIMPsWIMPsOscillationsOscillations
UndergroundUnderground
UnderwaterUnderwaterRadio,AcousticRadio,Acoustic
Air showersAir showers
Microquasars etc.
GZK
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1 pp core AGN (Nellen)2 p core AGN Stecker & Salomon)3 p „maximum model“ (Mannheim et al.)4 p blazar jets (Mannh)5 p AGN (Rachen & Biermann)6 pp AGN (Mannheim)7 GRB (Waxman & Bahcall)8 TD (Sigl)9 GZK
Diffuse Fluxes: Predictions and Bounds
Mannheim & Learned,2000
MacroBaikalAmanda
9
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2. Detection Methodsand Projects
A. Underwater/Ice Cherenkov TelescopesB. Acoustic DetectionC. Radio DetectionD. Detection by Air Showers
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Underwater/Ice Cherenkov Telescopes
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cascademuon
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AMANDA Event
Signatures:Muons
AMANDA Event
Signatures:Muons
+ N + X
CC muon neutrinointeraction track
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AMANDA Event
Signatures: Cascades
AMANDA Event
Signatures: Cascades
CC electron and tau neutrino interaction:
(e,,) + N (e, ) + X
NC neutrino interaction:
x + N x + X
Cascades
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4-string stage (1996)
First underwater telescopeFirst neutrinos underwater
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E2 < 1.9 10-6 cm-2 s-1 sr-1 GeV
Limit on diffuse fluxes
1998
e cascades Upgrade with only 22 PMTs factor 4 in sensitivity
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NT-200192 PMT>15 GeV
NT-Km3~ 1300 PMT> 100 TeV
NT-200+214 PMT
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AMANDA-II
depth AMANDA
Super-K
DUMANDAmanda-II:677 PMTsat 19 strings
(1996-2000)
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1 km
2 km
SPASE air shower arrays
calibration of AMANDA angular resolution and pointing !
resolution Amanda-B10 ~ 3.5°
results in ~ 3° for upward moving muons
(Amanda-II: < 2°)
Unique:spase-amanda
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Atmospheric Neutrinos, 97 data
vertically up horizontally AMANDA sensitivity understood down to normalization factor of ~ 40% (modeling of ice ...)
~ 300 events
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Preliminary limits (in units of 10-15 muons cm-2 s-1): Cas A: 0.6 Mk421: 1.4 Mk501: 0.8 Crab: 6.8 SS433: 10.5
Point Sources Amanda II (2000)
1328 events
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Expected sensitivity AMANDA 97-02 data
4 years Super-Kamiokande
8 years MACRO
170 days AMANDA-B10
-90 0-45 9045
10-15
10-14
cm-2 s
-1
declination (degrees)
southern sky
northern sky
SS-433
Mk-421 / ~ 1
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Amanda 97: Upper limit on the diffuse flux of h.e. upward muon neutrinos
E2 < 0.9 10-6 GeV-1 cm-2 s-1 sr-1
„AGN“ with 10-5 E-2 GeV-1 cm-2 s-1 sr-1
full: experiment
dotted: atmos.
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Diffuse fluxes: theoretical bounds and experimental limits
atmosphärische N
eutrinos
W&B W&B
MPRMPR
DUMAND test string
FREJUS
NT-200+
AMANDA-II
IceCube
NT-200AMANDA-B10
MACRO
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2002 real time analysis
Daily transmission ~ 1 GB via satelliteFull data to tape (available next polar summer)
Monitoring shifts in home labs
From 02/03:Iridium connection for supernova alarm
event June 14
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IceCube
1400 m
2400 m
AMANDA
South Pole
IceTop
- 80 Strings- 4800 PMT - Instrumented
volume: 1 km3
- Installation: 2004-2010
~ 80.000 atm. per year
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cos
Ae
ff /
km2
Effective area of IceCube
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Mediterranean Projects
4100m
2400m
3400mANTARESNEMO NESTOR
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NESTOR
Site: Pylos (Greece), 3800m depth towers of 12 titanium floors each supporting 12 PMTs
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7 NESTOR towers → 75 000 m² at 1 TeV
1 NESTOR tower + 3 DUMAND strings
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-2400m
40 km
Submarine cable
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ANTARES Design
2500m2500m
300m300mactiveactive
Electro-opticElectro-opticsubmarine cablesubmarine cable ~40km~40km
Junction boxJunction box
Readout cablesReadout cables
Shore stationShore station
anchoranchor
floatfloat
Electronics containersElectronics containers
~60m~60mCompass,Compass,tilt metertilt meter
hydrophonehydrophone
Optical moduleOptical module
Acoustic beaconAcoustic beacon
~100m
10 strings12 m between storeys
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ANTARES Performance
Very good angular accuracybelow 3 TeV angular error is dominatedby kinematics, above 3 TeV by recon-struction error (~ 0.4°)
Effective area: ~ 10 000 m2 at 1 TeV ~ 50 000 m2 at 100 TeV
after cutsagainst BG
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NEMO Neutrino Mediterranean Observatory
abs. length ~70 m80 km from coast 3400 m deep
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NEMO 1999 - 2001 Site selection and R&D
2002 - 2004 Prototyping at Catania Test Site 2005 - ? Construction of km3 Detector
ANTARES 1996 - 2000 R&D, Site Evaluation 2000 Demonstrator line 2001 Start Construction
September 2002 Deploy prototype line December 2004 10 (12?) line detector complete 2005 - ? Construction of km3 Detector
NESTOR 1991 - 2000 R & D, Site Evaluation Summer 2002 Deployment 2 floors Winter 2003 Recovery & re-deployment with 4 floors Autumn 2003 Full Tower deployment 2004 Add 3 DUMAND strings around tower 2005 - ? Deployment of 7 NESTOR towers
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Acoustic Detection
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d
R
Particle cascade ionization heat pressure wave
P
t
50s
Attenuation length of sea water at 15-30 kHz: a few km(light: a few tens of meters)
→ given a large initial signal, huge detection volumes can be achieved.
Threshold > 10 PeV
Maximum of emission at ~ 20 kHz
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Renewed efforts along acoustic method for GZK neutrino detection
Greece: SADCO Mediterannean, NESTOR site, 3 strings with hydrophones
Russia: AGAM antennas near Kamchatka:existing sonar array for submarine detection
Russia: MG-10M antennas: withdrawn sonar array for submarine detection
AUTEC: US Navy array in Atlantic:existing sonar array for submarine detection
Antares: R&D for acoustic detection
IceCube: R&D for acoustic detection
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AUTEC array in Atlantic
Atlantic Undersea Test and Evaluation Center
52 sensors on 2.5 km lattice (250 km2) 4.5 m above surface 1-50 kHz !
Threshold ~ 100 EeV
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Radio Detection
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e + n p + e-
e- ... cascade
relativist. pancake ~ 1cm thick, ~10cm
each particle emits Cherenkov radiation
C signal is resultant of overlapping Cherenkov cones
for >> 10 cm (radio) coherence
C-signal ~ E2
nsec
negative charge is sweeped into developing shower, which acquiresa negative net chargeQnet ~ 0.25 Ecascade (GeV).
Threshold > 10 PeV
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RICE Radio Ice Cherenkov Experiment
firn layer (to 120 m depth)
UHE NEUTRINO DIRECTION
300 METER DEPTH
E 2 · dN/dE < 10-4 GeV · cm-2 · s-1 · sr-1
20 receivers + transmitters
at 100 PeV
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Natural Salt Domes
Potential PeV-EeV Neutrino Detectors
SalSA Salt Dome Shower Array
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ANITA Antarctic
Impulsive
Transient
Array
Flight in 2006
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GLUE Goldstone Lunar Ultra-high Energy Neutrino Experiment
E2·dN/dE < 10-4 GeV·cm-2·s-1·sr-1
Lunar Radio Emissions from Inter-actions of and CR with > 1019 eV
1 nsec
moon
Earth
Gorham et al. (1999), 30 hr NASA Goldstone70 m antenna + DSS 34 m antenna
at 1020 eV
Effective target volume~ antenna beam (0.3°) 10 m layer
105 km3
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Measured & Predicted Radio Limits
• Radio is competitive with optical km3 arrays for E >10 PeV
• Required detection times are small, a benefit of the enormous volumes radio detectors can view
• But: background ??
AMANDA-II 3 years expected
km3 , 3 years expected
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Detection of neutrino induced
air showers
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el.-magn.cascade
from e
hardmuons
from CR
AGASA 2001:
< 10-5 GeV·cm-2·s-1·sr-1
for E > 10 EeV
Far inclined showers ( thousand per year)
Hard s
Atm
osphere
• Flat and thin shower front• Narrow signals• Time alignment
Deep inclined showers (~ one per year?)
Atm
osphere
Soft s + e.m.
• Curved and thick shower front• Broad signals
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Predicted Auger SensitivitiesPredicted Auger Sensitivities
Comparable to 3-year optical km3 limit
Mass for and e
~ 15 Gigatonssensitivity 3·10-7 GeV·cm-2·s-1·sr-1
Skimming high acceptance at ~EeV !
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Horizontal Air Showers seen by Satellite
500 km
60 °
E > 1019 GeV
Area upto 106 km2
Mass upto 10Tera-tons
Horizontal air shower initiated deep in atmosphere
1 - 20 GZK ev./y
5 - 50 TD ev./y
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Orbiting Wide-angle Light-collectors
OWL
Extreme Universe Space Observatory
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5. The next decade
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RICE AGASA
Amanda, Baikal2002
2004
2007
AUGER
Anita
AABN
2012
km3
EUSOAugerSalsa
GLUE
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Mediterannean
South Pole
Fraction of time sky below horizonPoint sources:detector South + detector North
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-90 0-45 9045
10-15
10-14
cm-2 s-1
SS-433
Mk-501
/ ~ 1
10-17
10-16
2001
2007
2003
2012
Expected sensitivitiesto steady point sources
GX339-4
„typical“ predictions for AGN, SNR, ... „typical“ predictions for AGN, SNR, ...
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0.1 km² and 1 km² detectors underwater and ice