Alternative%20Detection%20Methods%20for%20Highest%20Energy%20Neutrinos

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Alternative Detection Methods for Highest Energy
Neutrinos Rolf Nahnhauer DESY
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Energies and Fluxes

• Stecker Salamon (AGN)
• Protheroe (AGN)
• Mannheim (AGN)
• Protheroe Stanev (TD)
• Engel, Seckel Stanev

typical energy gt 1017-18 eVtypical fluxE2
lt 10-7 GeVcm-2s-1sr-1
p gCMB ? p .
standard candle !
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?GZK Event Rates
Combination of results of different experimental
techniques may give indications soon, but need
larger detector volumes from ? existing
technologies ?abs ? O(100m), scale,
improve, reduce cost ? radio detection
?abs ? O(1000m), first promising results
? acoustic detection ?abs ? O(1000m),
still mainly RD
from D. Saltzberg astro-ph/0501364
see B. Price, Astrop. Phys. 5 (1996) 43
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From IceCubeto IceCube-Plus?
F.Halzen, D.Hooper astro-ph/0310152 JCPA 0401
(2004)002
Add strings to existing IceCube detector at
larger distances Consequences High threshold
Large detection volume Profit from well
understood technology
?
?GZK/year rings strings ?d/m shower
muons IceCube 0 0
0 0.6 0.8 IceCube-Plus
1 13 300 1.1
1.1 HyperCube 4 81
500 4.5 2.8
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Radio Detection I
G.A. Askaryan JETP 14 (1962) 441 Excess negative
charge of an electron-photon shower and its
coherent radio emission
Saltzberg et al., PRL 86 (2001) 2802 Confirme
effect by accelerator measurements in silica sand
dc
Coherence condition dc ?10cm lt
?radio 300 MHz ? ? 100 cm
Signal power E2 Np2
Lc
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The In-Matter Approach I
Absorption strong function of temperatureFor
cold ice 0.1-1.0 GHz bestAllows radio signal to
travel gt 1 km
Deployed at South Pole1996-1998
RICE Radio Ice Cherenkov Experiment
? Uses AMANDA holes? 18 Receivers (10 cm
dipole) ? 5 Transmitters ? 3 Horns (INR mark)?
100-300 m depth? 200x200x200 m3 cube ? DAQ,
PCs, Pulse Generator ? 1 dry hole
AMANDA
South Pole
From D. Besson, talk 09/2003
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surface reflections (03 data)
RICE Radioglaciology
astro-ph/0306408
measure EM wavespeed variation through firn
Index of refraction measurement (2003)
0 m
-90 m
Bedrock/2850m
Long range attenuationBottom echo visible
through 5.6 km!(20 dB noise reduction
averaging)
From D. Besson, talk 03/2004
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RICE Neutrino-Detection
RICE CUBE 20??
astro-ph/0306408, 3500 hours livetime
-500 m
-1000 m
-1500 m
-2000 m
-2500 m
project still under discussionholes may be
separate from IceCubeVeff growth 10-25
From D. Besson, talk 03/2004
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Goldstone Lunar Ultra-high energy neutrino
Experiment
The Bottom-Up Approach
Original idea by Askaryan in 1962 paper

From P.Gorham,talk Hawai 02/2004
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GLUE
effective target volume 100,000 cubic km
! limited primarily by livetime (120 hours)
typical event look for 6 ? above thermal noise in
all channels no event in 120 hours
astro-ph/0310232v3 05/2004
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The Top-Down Approach I
Fast On-orbit RadioTransient Experiment
N. Lethinen et al., astro-ph/0309656v2 10/2003
FORTE

• Pegasus launch in 1997
• 800 km orbit, 3 year planned life
• Scientific program in lightning related
  atmospheric discharges
• 30-300 MHz range
• 4 M triggers recorded 9/97-12/99

Look for RF signals from Greenland Ice
Also P.Gorham,talk Hawai 02/2004
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Limits from FORTE and GLUE
N. Lethinen et al.,astro-ph/0309656 v2 10/2003
P. Gorham et al.,astro-ph/0310232v3 05/2004
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The Top-Down Approach II
Radio Detector Balloon Flight
AntarcticImpulsiveTransientAntenna
From S. Barwick, APS talk 04/2004
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ANITA
From S. Barwick,APS talk 04/2004
NASA funding started 2003 for first launch in
2006 Phase A approval for SMEX ToO mission
ANITA- lite
18 days at float altitude 1.25
revolutions landing near Mawson Station Data
recovered in Feb 04
Piggyback on TIGER Launch Dec 03 2 Receiver
Horns RF Survey of Antarctica
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ANITA-lite
From S. Barwick,APS talk 04/2004
and astro-ph/0411007
Timing
BG event
Ground antenna transmitscalib. pulse to
Anita-lite _at_40km
Duration is too large for ?
Signal
?t 0.12 ns per Antenna
512ns
Expected for ANITA ?? 0.5 deg, ?? 2 deg
Initial scan of data reveals no obvious ? signal
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Radio Detection II
radio signals from air showers
Jelley et al. 1965, Allan 1971, H. Falcke, P.
Gorham, astro-ph/0207226
deflection of electron-positron pairs in the
earths magnetic fieldhighly beamed pulses of
synchrotron radiation coherent emission at low
frequencies
radio detectors ? see shower development
? observe 24 hrs/day ? have low cost ?
Ethr gt 1016eV ? efficient ?e, ?? detection
Figure from G. Cusumano
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The LOPES Project
2003 10 antennas at KASCADE ( E0 gt 1016 eV) ?
technology studies
one candidate event
? energy ? 1017 eV ? EAS core inside antennas ?
signals in 8 of 10 antennas ? signal is coherent
2005 30 antennas at KASCADE-Grande, O(1000)
events gt 100 PeV
From A. Haungs et al., TEXAS Symposium, Stanford
Dec. 2004
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CODALEMA
6 Antennas at Nançay Radio observatory1-100 MHz
D. Ardouin et al. ECRS 2004 Florence,
Xx
look for radio emission of cosmic air showers
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Acoustic Detection
? abs(light) ? O(100m), ?abs(sound) ?
?abs(radio) ? (1000m)
G.A. Askaryan, At. Energ., vol.3, no.8, (1957)
p.152 Askaryan, Dolgoshein, Kalinovsky, NIM
164(1979) 267
The Thermo-Acoustic Model
? Particle cascades produce pressure
pulses? Pressure amplitude measures incoming
energy ? Pressure distribution measures
incoming direction? Frequency 10-100 kHz ?
Signal power E2
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First Proposal DUMAND
Calculated signal strength in H2O Learned,
Phys.Rew. D 19(1979) 3293
Beam test with 200 MeV protons Sulak et al. NIM
161(1979) 203

detector hydrophone Ethr ? 21015 eV ,
(for R 8cm) P 0.2 dyn/cm2
E1016eV,R10m,f16kHz P 0.810-3 dyn/cm2
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Todays Activities at Different Sides
Group Location Activities
Stanford Bahamas data taking, signal processing, calibration , simulation
Moscow, INR1 Kamtschatka,Black Sea signal processing, calibration , simulation
Moscow, INR2, Irkutsk Baikal signal processing, noise studies
ITEP Baikal, Mediterranean detector RD, accel. tests, signal processing, noise studies
Marseille Mediterranean detector RD, calibration, noise studies, simulation,
Erlangen Mediterranean detector RD, accel. tests, calibration, simulation
Rom, Catania Mediterranean installation RD, noise studies, simulation
Pisa, Corbino, Firenze, Genova Mediterranean detector RD, DAQ
Valencia Mediterranean detector RD
Sheffield Scotland, Mediterranean simulation, signal processing , calibration
U. Texas Hockley detector RD, attenuation studies, material studies
Berkeley, DESY, Uppsala South Pole detector RD, accel. tests, material studies, simulation
For details see e.g. R. Nahnhauer,
astro-ph/0411715 V. Bertin,
HEAPNET meeting Roma 11/02/2005
http//www.roma1.infn.it/exp/ams/
11Febbraio05/Agenda.html
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First experiment with published flux limit
SAUND
Signal simulation E ? ? 1020 eV
AUTEC
Refraction important for signal tracing
SAUND7 km2
J. Vandenbroucke et al., astro-ph/0406105
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SAUND
Data Analysis
only simulated events in fiducial volume
(1023eV,1024 eV,1025eV)
J. Vandenbroucke et al., astro-ph/0406105
Data taking65 106 eventsin 195 days
Background rejection
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Projects of the next decade

• ? observe gt 10 events/year from GZK ? flux
• ? Veff 50 km3
• ? target material water, ice, salt, rock?
• profit from combination of different
  detections methods
• optical-acoustic-radio
• in background reduction, cross calibration,
  detection sensitivity,

All Radiation EeV Neutrino detection Arrays
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The Water ARENA
Acoustic
1000 hydrophone array for Mediterranean 3
hydrophones per cluster( sensor distance 50 m
)300 m grid spacing
red line incident neutrino
(7.21019 eV)red cube deposited
energy of ? - interactionyellow points
hydrophonesgreen cubes signal hits
From L. Thompson, unpublished And U. Katz, ApPEC
Workshop 2003
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Water ARENA Sensor RD
selfmade
Erlangen cheap selfmade hydrophones sensitivity
6x commercial S/N ? 10

commercial
From P. Kollmannsberger, DPG 2004
Pisa, Firenzefibre acoustic sensors
spectral response to a 65 kHz loud-speaker
modulation (Mach-Zender OPD 150 m)
From M.Morganti, Roma 2005
pressure wave on fibre ? modulation of cavity
size, leading to modulation of laser wavelength
detectable by interferometer
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A Water ARENA Test Site
Shore laboratory port of Catania
A fully equipped facility to test and develop
technologies for the Mediterranean km3
Underwater test site 25 km E offshore
Catania 2000 m depth
cable 10 OF 6 conductors
2004-2006
From G. Riccobene for this workshop
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First tests The NEMO - O?DE (Ocean noise
Detection Experiment)
Sperm whales clicks

• 4 hydrophones
• 2 (10 Hz - 40 kHz) 2 (1 kHz - 40 kHz)
• Digitization (24 bits 96 kHz) and electro-optical
  translation
• Continuous monitoring from shore

From G. Riccobene for this workshop
Successfully deployed on 23 Jan 2005
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The Air ARENA
AUGER Radio
1EeV air shower
4 km
If LOPES RD successful ? add radio detectors
to AUGER
radio beam
2 km
vertical 1017 eV air shower
center100m250m dataAllan and Prah
1mV/m/Mhz
1
50 km
A. Horneffer et al., SPIE 2004
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Many Gulf coast salt domes3-4 km diameters, 5-10
km depths typical
The Salt ARENA I
From M. Chiba, NANP-Dubna 2003
many big salt domes around the world
Canada 8x5 km2
Iran, 7km diameter
Typical salt dome RF loss similar to ice at
-40 C 2.5 times more dense ? build
radio detector array
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Basic array geometry simulatedP. Gorham talk at
SLAC meeting
The Salt ARENA I
Meeting at SLAC Feb/05 SalSA Collaboration
bornU-Hawaii,UCLA, SLAC,
Phase 1 look for right locationdeploy test
strings in a few holes study attenuation, noise
etc in-situ
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2
2.5 km3 array with 225 m spacing 122144 strings,
1231728 antenna nodes 12 antennas per node, dual
polarization 300 km3 sr at 1 EeV threshold 1017
eV, few 100s antennas hit at 1 EeV, gt1000 hits
at 10 EeV Rate claim at least 10 events per year
from rock-bottom minimal GZK predictions
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Depth (km)
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• Halite (rock salt)
• La(lt1GHz) gt 500 m w.e.
• Depth to gt10km
• Diameter 3-8 km
• Veff 100-200 km3 w.e.
• No known background
• gt2p steradians possible

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6
7
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The Salt ARENA I
Add acoustic detector array to SalSA?
Theoretical expectations
Water Ice Salt
? g/cm3 1 .9 2.1
Vs m/s 1450 3800 4500
P/Pwater 1 10 25
f/fwater 1 3 6
eff. abs km ? 7 ? km
noise large small ? small ?
f 1 100 kHz, fres 150 kHz
1 crack seen by 12 detectors pressure waves
shear waves
Signal attenuation ?att 1/a S Ae-ar/rn n 2
used ?att 170 m ! Signal location lt 1 m
From B.Price at SLAC meeting 02/05
Need measurements
learn from geophysicists
T. Spies, J. Eisenblätter, J.Manthei,Z. f.
angewandte Geologie, H2, 2002, 30and references
therein
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The Salt ARENA II
LOFAR
interferometer in frequency range of 10 - 200
MHz array of 100 stations of 100 dipole
antennas baselines of 10 m to 400 km All-Sky
monitor transient events
LOFAR ZESANA
http//www.lofar.org
Zuidwending
Detect UHE ?s using rock salt in Northern Europe
(Groningen) Monitor UHE CRs with
LOFAR Develop radar techniques for salt
domes techniques to install antennas in salt domes
Onstwedde
?7,5 km?
salt pillars
Zechstein salt
Zuidwending
From A. M. van den Berg, SLAC meeting 02/05
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The Ice ARENA
IceCube Collaboration Study a hybrid
optical-radio-acoustic array Idea behind try to
cross calibrate the detector,if discovery is
made with one technique, confirmation with
different technique necessary
acoustic array alone
IC
?abs min Nch GZK (HS) events/year
1 km 4 min 0.5
1km 4 max 1.5
6 km 4 min 18
6 km 4 max 54
o radio acoustic? optical (IceCube)? ora
(IceCube)
example0.5 km spacing1.5 km strings91
stringsVeff 58 km3
acoustic noise
From J. Vandenbroucke,IceCube meeting Uppsala
10/04
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The Ice ARENA
Radio antennas for ice available and tested
(RICE)Acoustic glaciophones under development
Testrun at proton beam
Etot 5.6 PeV 1.7 EeV E min (1m) ? 10 PeVP
min 10 mPa
Calibration (until now only in water) reference
hydrophone Sensortech SQ03 -163.30.3 dB re
1V/µPa
iron ball
Improvement (S/N)ib 50 (S/N)gb 15
glass ball
From S. Böser et al., to be published
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The Ice ARENA
Ice properties for propagation of light measured
(AMANDA)Ice properties for propagation of radio
signals measured (RICE)Ice properties for
propagation of sound waves still to be
measured urgent requirement ? study ambient
noise ? measure absorption length
test foreseen for season 05/06
Proposal use 3 holes diameter
6 depth 400 m 7 sensors per hole large
variation of ice properties at the surface ?
non-equal spacing 7 transmitters per hole no
possibility for transmitter allingment ?
azimuthal symmetry
x
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Summary Conclusions
For the observation of the tiny neutrino fluxes
above 1018 eV ? Optical detection
techniques seem to reach their limits ?
Radio detectors start to become sensitive
? Acoustic detectors have a big revival but
still need RD Further progress would profit
from ? Combination of different detection
techniques in one project ? Dedicated
experiments at large scales ? Network of
worldwide cooperation
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International ARENA Workshop May, 17 19
2005 DESY, Zeuthen, GERMANY http//www-zeuthen.de
sy.de/arena