Upload
ernest-noah-lane
View
219
Download
2
Tags:
Embed Size (px)
Citation preview
Alternative Detection Methods for Highest Energy Neutrinos
Rolf Nahnhauer – DESY Zeuthen
1
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from D. Saltzberg (unpublished)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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 3
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
a
From IceCubeto IceCube-Plus?
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 4
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 |
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 5
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 6
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
From D. Besson, talk 03/2004
astro-ph/0306408
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 7
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
From D. Besson, talk 03/2004
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 8
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 9
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 10
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 11
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 12
Limits from FORTE and GLUE
P. Gorham et al.,astro-ph/0310232v3 05/2004
N. Lethinen et al.,astro-ph/0309656 v2 10/2003
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 13
The Top-Down Approach II
Radio Detector Balloon Flight
AntarcticImpulsiveTransientAntenna
From S. Barwick, APS talk 04/2004
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 14
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 15
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 16
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 17
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 18
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 19
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 20
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 21
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 22
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 23
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 24
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 25
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 26
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 :
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 27
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
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 28
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 29
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
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 30
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 31
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 32
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 33
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
|
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 34
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 35
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
a
a -2004, June 18, 2004 Rolf Nahnhauer – DESY Zeuthen 36
PMT array
pixel array