alternative detection methods for highest energy neutrinos rolf nahnhauer – desy zeuthen 1...

Alternative Detection Methods for Highest Energy Neutrinos

Rolf Nahnhauer – DESY Zeuthen

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Introduction

Cherenkov

Radio I Radio II Acoustic Conclusion

a -2004, June 18, 2004

Energies and Fluxes•Stecker & Salamon (AGN)•Protheroe (AGN)•Mannheim (AGN)•Protheroe & Stanev (TD)•Engel, Seckel & Stanev

p + p + CMBCMB + …. + ….

standard candle !

typical energy: > 1017-18 eV

typical flux*E2:

< 10-7 GeVcm-2s-1sr-1

a

a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 2

GZK Event Rates

from D. Saltzberg (unpublished)

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 R&D

see B. Price, Astrop. Phys. 5 (1996) 43

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F.Halzen, D.Hooper

astro-ph/0310152

JCPA 0401 (2004)002

Add strings to existing IceCube detector at larger distances

Consequences:

High threshold >10 PeV

Large detection volume

Profit from well understood technology

GZK/year

rings +strings d/m shower muonsIceCube 0 0 0 0.6 0.8IceCube-Plus 1 13 300 1.1 1.1HyperCube 4 81 500 4.5 2.8

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From IceCubeto IceCube-Plus?


Radio Detection IG.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

Coherence condition:

dc 10cm < radio

300 MHz = 100 cm

Signal power ~ E2 ~ Np2

| d

c |

| Lc |

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The In-Matter Approach I

RICE :Radio Ice Cherenkov Experiment

Use 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

Deployed at South Pole1996-1998:

From D. Besson, talk 09/2003

Absorption strong function of temperatureFor cold ice 0.1-1.0 GHz bestAllows radio signal to travel > 1 km

AMANDA

South Pole

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RICE: Radioglaciologymeasure EM wavespeed variation through firn

Index of refraction measurement (2003)0 m

-90 m

surface reflections (03 data)

Long range attenuation:Bottom echo visible through 5.6 km!(20 dB noise reduction [averaging])

Bedrock/2850m


astro-ph/0306408

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RICE: Neutrino-Detection

astro-ph/0306408, 3500 hours livetime

RICE – CUBE 20??

-500 m

-1500 m

-1000 m

-2000 m

-2500 m

project still under discussionholes may be separate from IceCubeVeff growth ~10-25


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The In-Matter Approach IIRadio Detection in Natural Salt Domes

From P.Gorham, talk Hawai 02/2004see also: NIM A490 (2002)476

From M. Chiba, NANP-Dubna 2003

Typical salt dome: RF loss similar to ice at -40° C 2.5 times more dense

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SALSA: SALtbed Shower ArrayMonte Carlo Design Studies:D.Saltzberg et al., Proc. SPIE V4858(2003)191

From M. Chiba, NANP-Dubna 2003

S 125 : 125 antennas in 1 km3

S1000 : 1000 antennas in 1 km3 S1000L : 1000 antennas in 8 km3

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Goldstone Lunar Ultra-high energy neutrino Experiment

effective target volume: ~ 100,000 cubic km !limited primarily by livetime (120 hours)

astro-ph/0310232v3 05/2004

Original idea by Askaryan in 1962 paper

1 GLUE:

The Bottom-Up Approach From P.Gorham,talk Hawai 02/2004

typical event

look for 6 above thermal noise in all channels

no event in 120 hours

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The Top-Down Approach I

FORTE: Fast On-orbit RadioTransient Experiment

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

N. Lethinen et al., astro-ph/0309656v2 10/2003

Also P.Gorham,talk Hawai 02/2004

Look for RF signals from Greenland Ice

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Limits from FORTE and GLUE

P. Gorham et al.,astro-ph/0310232v3 05/2004

N. Lethinen et al.,astro-ph/0309656 v2 10/2003

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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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NASA funding started 2003 for first launch in 2006

Phase A approval for SMEX ToO mission

ANITA

ANITA- lite:Piggyback on TIGERLaunch Dec ‘032 Receiver HornsRF Survey of Antarctica

18 days at float altitude1.25 revolutionslanding nearMawson StationData recoveredin Feb 04

From S. Barwick,APS talk 04/2004

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BG event

Initial scan of data reveals no obvious signal

Duration is too large for

512ns

ANITA-liteTiming

Ground antenna transmitscalib. pulse to Anita-lite @40km

t = 0.12 nsper Antenna

Expected for ANITA: ~ 0.5 deg, ~ 2 deg

From S. Barwick,APS talk 04/2004

~Signal

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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 earth’s magnetic field

highly beamed pulses of synchrotron radiation

coherent emission at low frequencies

Radio Detection II

Figure from G. Cusumano

radio detectors see shower development observe 24 hrs/day have low cost Ethr > 1016eV efficient e, detection

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If R&D successful add radio detectors to AUGER

4 km 1EeV air shower

radio beam

2 km

50 km

1mV/mMhz

The LOPES Project2003 :10 antennas at KASCADE( E0 > 1016 eV) noise studiesAim: ~100 antennas at KASCADE-Grande, O(1000) events > 100 PeV

first candidate event:

1

energy 1017 eV EAS core inside antennas signals in 8 of 10 antennas signal is coherent From A. Haungs – talks Bremen, Karlsruhe, 02-03, 2004

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CODALEMA:

COsmic Detector Array Logarithmic Electro Magnetic Antennas

O.Ravel et al.,astro-ph/0306255

6 Antennas at Nançay Radio observatory1-100 MHz

look for radio emission of cosmic air showers

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Acoustic Detection abs(light) O(100m), abs(sound) abs(radio) (1000m)

The Thermo-Acoustic Model :

G.A. Askaryan, At. Energ., vol.3, no.8, (1957) p.152Askar´yan, Dolgoshein, Kalinovsky, NIM 164(1979) 267

● Particle cascades produce pressure pulses● Pressure amplitude measures incoming energy● Pressure distribution measures incoming direction● Frequency 10-100 kHz

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First Proposal: DUMANDCalculated signal strength in H2OLearned, Phys.Rew. D 19(1979) 3293

Beam test with 200 MeV protonsSulak et al. NIM 161(1979) 203

E=1016eV,R=10m,f=16kHz P = 0.8*10-3 dyn/cm2

detector: hydrophone Ethr 2*1015 eV , (for R = 8cm)

P = 0.2 dyn/cm2

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Todays Activities at Different SidesSee also http://hep.stanford.edu/neutrino/SAUND/workshop/slides/

group experiment Location activities

Stanford SAUND Bahamas data taking, signal processing, calibration , simulation

INR1AGAM MP10

Kamtschatka,Black Sea

signal processing, calibration , simulation

INR2, Irkutsk Baikal Lake Baikal signal processing, noise studies

ITEPBaikal, Antares

Lake Baikal, Mediterranean

detector R&D, accel. tests, in situ tests at Baikal, signal processing, noise studies

Marseille Antares Mediterraneandetector and installation R&D, calibration, noise studies, simulation,

Erlangen Antares Mediterranean detector R&D, accel. tests, calibration, simulation

Rom, Catania NEMO Mediterranean installation R&D, noise studies, simulation

Un. Kingdom Rona, Antares Scotland, Med. simulation, signal processing , calibration

U. Texas Salt Dome Hockley detector R&D, attenuation studies, material studies

Berkeley, DESY, Uppsala

IceCube South Pole detector R&D, accel. tests, material studies, simulation

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SAUND I Study of Acoustic Ultrahigh-energy Neutrino Detection

AUTEC

SAUND7 km2

Signal simulation E 1020

eV

J. Vandenbroucke et al., astro-ph/0406105

Refraction important for signal tracing

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SAUND II

Background rejection:

Data Analysisonly simulated events in fiducial volume (1023eV,1024 eV,1025eV)

firstfluxlimit from acoustic detector

J. Vandenbroucke et al., astro-ph/0406105

Data taking:65 *106 eventsin 195 days

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ITEP Moscow IV.I. Albul et al. Instr. and Exp. Techn. 44 (2001)327

beam: ITEP Moskau125MeV, 200 MeV p target : H2Odetector: hydrophone

Am

pli

tud

e

Am

pli

tud

e

Proton beam

Time [mks]

Ethr 1016 eVP [dyn] = 2.3*10-14 Eb

0.78 [eV]

P

Proton beam measurements Acoustic signal simulation

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An example of detected sound(hydrophones H1-H4,G7,G8)

Level o f acoustic no iseat Baika l for time period from 29 M arch to 2 April of 2002 yearH ydrophones of the antenne : #1(depth 3 m ) #2(depth 8 m ) #3(depth 13 m) #4(depth 18 m)and remote hydrophone : #5 (depth 3 m )

0 100 200 300 400 500 600 700 800 900 1000 1100 1200

Time, [current files]

0

20

40

60

80

100

120

140

160

180

200

220

240

260

me

an a

mp

litu

de

of s

ign

als

, [co

un

ts]

0

20

40

60

80

100

120

140

160

180

200

220

240

260

280

300

320

мП

а

Acoustic noise from Baikal water

/rad

sin

3 “clusters” = 90º surface noise = 0º ??? = -10º ???noise channeling below ice due to temperature gradient ?

time/msec

EASITEP Moscow II

piezo: -180 dB

Sensitive hydrophone manufacturing Experiments at Lake Baikal

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Marseille Study of ambient noise

Use French navy tracking array

Data taking campaign in June 2001: 8 hydrophones @ 1500 and 2500 m sampling frequencies 250 kHz filters window 100-100 kHz 3Gbytes of data, but many uncertainties should be redone soon

Measure in IFREMER pool

receivers

emitter

Autonomous acquisition system to characterize the ambient noise of the ANTARES site and to evaluate the feasibility of acoustic detection.

From V.Bertin, talk Stanford 09/2003

from ITEP Moscow

Acoustic pinger @ 4.5 kHz

sea conditions with 25-30 knots speed

Under construction :

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Erlangen Tests of the Thermoacoustic Model

177 MeV protonsenergy deposition in H2O Testrun at Theodor Svedberg Laboratory Uppsala 02/2004

Observe typical bipolar signal in agreement with simulation

Performed detailed studies oftemperature dependence of signal

zero transition:at 4.6 C not at 4.0 C

Data agree in general with thermoacoustic predictions

aFrom S.Kuch, K. Graf,DPG-talk 04/2004


UK Detector simulation

1000 hydrophone array for Mediterranean

3 hydrophones per cluster( sensor distance : 50 m )

300 m grid spacing

red line : incident neutrino (7.2*1019 eV)red cube : deposited energy of - interactionyellow points : hydrophonesgreen cubes : signal hits From L. Thompson, unpublished

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U.Texas Acoustic Signals in SaltTest measuremenrs in Hockley mine use piezo transmitter and receiver Kistler AE-Piezotron 8152B150 – 400 kHz frequency range

Press sensors against wall of 2.5’’ borehole

Distance to transmitterbetween 3 m and 20 m

Observe logitudinal waves and shear waves :

cp = 4337±84 m/s, cs = 2000±220 m/s

Aout ~ Ain

need calibration,expect Asalt >> AH2O

now attenuation under study

need sensor for lower frequency range

aFrom M. Fink, talk Stanford 09/2003,N. Kirby, Senior Thesis 2004


South Pole I

Expectations water*) ice**)

vs[m/sec] 1480 3900f [kHz] 25 65P[mPa*m/PeV] .26 2.4

Pice/Pwater = 9.2

(*) at 20º C, (**) at -40° C

Uppsala 19.-26.1.2003Uppsala 14.-21.2.2004

Etot = 5.6 PeV – 1.7 EeV

Testruns at a Proton Beam

For -cascades:

Pice/Pwater = 10.

threshold at ~1 m distanceE min 10 PeV

Atot

A1

bg

Atot

A1

Q/nC T/ºC

Observable pressure : ~10 mPaprecise calibration still open

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South Pole II

Deploy ≥ 2 acoustic test strings at South Pole

Depth : 300 m – 450 m

Sensors : own developmentbeam tested

Noise limitations :

Urgent requirement: study ambient noise measure absorption length

12 cm glass ball 12 cm iron ball

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Summary + ConclusionsFor 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 R&D

Further progress would profit from

Network for worldwide cooperation

Combination of different detection techniquesin one project

Dedicated experiments at large scales

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Acoustic andRadio Echoing of NeutrinoAvalanches

Vc = 40km3

Veff > 70 km3

Material:Ice, Salt, Rock ?

ARENA

11 x 11 strings, 2 km long 1.6 km instrumented500 m horizontal grid50 m vertical distance for acoustic200 m vertical distance for radio

5 km

5 km

| 1

.6 k

m

|

small hole diameter1089 radio receivers3993 acoustic sensors below surface digitization low event ratessimple communication

0.4 km

|

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Thanks for helpful discussions and unpublished material to:

G. Anton, S. Barwick, D. Besson, S. Böser, H. Falcke, M.Fink, K. Graf, G. Gratta, A. Hallgren, F. Halzen, A. Haungs, U. Katz, P. Kollmannsberger, S. Kuch, J. Learned, B. Price, A. Rostovtzev, K. Salomon, D. Saltzberg, D. Seckel, C. Spiering, J. Stegmayer, L. Thompson, J. Vandenbroucke

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Sky monitorsfor Detection

EUSO, AUGER: elsewhere

AUGER Radio : later

From S.Dye - SAGENAP talk April 2004

All-sky Survey High-Resolution Air shower detector

Collaboration:

Japan, Taiwan,USA

New Detector concept:

Simultaneous detection of Cerenkov and Fluorescense light with high space resoultion

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PMT array

pixel array

alternative detection methods for highest energy neutrinos rolf nahnhauer – desy zeuthen 1...

Documents

radio detection ig

radio signal

existing icecube detector

afrom icecube

alternative detection

kmamandasouth pole aa

typical energy

icecube veff growth