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![Page 1: ANTARES: Towards Acoustic Detection of Highest Energy Neutrinos Kay Graf for the ANTARES Collaboration Erlangen Centre for Astroparticle Physics VLV T.](https://reader035.fdocuments.us/reader035/viewer/2022062717/56649e485503460f94b3b86f/html5/thumbnails/1.jpg)
ANTARES: Towards Acoustic Detection of Highest Energy Neutrinos
Kay Graf for the ANTARES Collaboration
Erlangen Centre for Astroparticle Physics
VLVT 09, Athens, Oct. 13th – 15th 2009
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Outline
• Motivation• The AMADEUS System• Positioning• Source Reconstruction
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 2
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Motivation
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 3
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Ultra-high Energy Neutrino Astrophysics
at energies above 1014-15eV:
• universe becomes opaque to
photons at Mpc range
• CR protons, nuclei are galactic up to
~1018eV, suffer GZK cut-off above
that
• neutrinos unabsorbed at all energies
→ sources exist to at least
3x1020eV
• UHE neutrinos are the only viable
messenger beyond the local
universe
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 4
vi
able
thr
ough
out
thes
e re
gion
s
P. Gorham
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Highest Energy Neutrinos
• astrophysics:
origin of UHECR
GZK neutrinos
• cosmology:
top-down scenarios
topological defects
• particle physics:
neutrino cross section
5Kay Graf (ECAP) – VLVnT 09, Athens – October 2009
log10(E[eV])1614 2418
TD
20 22
T. Karg, arXiv:astro-ph/0608312
10-4
10-8
10-6
10-10
Flu
x ×
E2 [e
V m
-2 s
-1 s
r-1]
water/iceCherenkovtelescopes
complementary techniques
for GZK : >100km2 ∙ 2∙ year detector needed
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(U)HE Detection Methods
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 6
neutrino cascadecascade
hydrophone arrayAcoustic Detection
water, ice, salt
att > 1km (water)
sonic wavesonic wave
radio radio CherenkovCherenkov
cascadecascade
antenna arrayRadio Cherenkov
ice, salt, rock
att ~ 1km (ice)
opticalopticalCherenkovCherenkov
PMT arrayOptical Cherenkov
water, ice
att < 100m
• balloon• satellite• telescope
+ hybrid detectors
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Acoustic Signal Properties
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 7
Ecasc= 1 EeV @ 1km
bipolar signal (~10kHz) with disk-like geometry
Acorne Coll. astro-ph/0704.1025
peak pressure
(mPa/EeV)
T. Karg, astro-ph/0608312v1
log10 (radial distance (m))di
stan
ce a
long
sho
wer
axi
s (m
) shower maximum
log10 (radial distance (m))
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Simulations of an Acoustic Detector
• strong dependence: Veff(Pthres)
• Pthres mainly given by ambient noise
• a threshold of 5mPa seems reachable in the deep-sea
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 8
T. Karg, arXiv:astro-ph/0608312
200 acoustic antennas/km3
Pthres
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The AMADEUS System
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 9
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The AMADEUS Project
Feasibility Study
• detector environment (hybrid)
• detector calibration functionality
• sensor design and positioning
• background studies
• signal processing techniques
integration of acoustic setup into the ANTARES neutrino telescope
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 10
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The ANTARES Neutrino Telescope
• optical Cherenkov Telescope
• 875 PMT• at 2500m water depth• Vinst~ 200 x 200 x 400 m3
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 11
ANTARESsite
F
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The AMADEUS System
• taking data since 5-Dec-2007
• completely installed since 30-May-2008
• acoustics on L12: data from 6-Sep to 24-Dec 2008
“pingers“ (acoustic RxTx) on each anchor
12Kay Graf (ECAP) – VLVnT 09, Athens – October 2009
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AMADEUS Facts
• characteristics- 36 sensors at 6 storeys
(1 – 350m distance, 34 active)- 16bit @ 250kSps sampling- ~ -125dB re 1V/Pa sensitivity- ~85-90% uptime
• data acquisition- all data to shore- raw: 20 MByte/s (1.5 TByte/d) - filtered: 0.3 MByte/s (4 GByte/d), up to now: 4
TByte - excellent stability of all DAQ parts
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 13
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Data Samples: Amplitude Histograms
noise at different sensors• gaussian profile• linear correlation between
sensors (factor ~ 99%)
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 14
noise and transient• additional tails• ~60dB S/N (SINAD), no
significant crosstalk
Sam
ple
s (p
er
AD
C c
ount)
Sam
ple
s (p
er
AD
C c
ount)
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Positioning
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 15
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Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 16
Positioning: Method for Reconstruction
use emissions from the ANTARES acoustic positioning system (not directly connected with AMADEUS)
→ positioning of individual sensors:• use absolute time from > 3 pingers:
| rreception – remission | = cs ¢ (treception – temission – toffset )
• treception by threshold crossing of signal envelope
• temission from positioning system
→ position/orientation by fitting storey geometry
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Positioning: Example
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 17
• 5 days of data• completely independent derivation of heading
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Acoustic Modules (AMs)
Piezo sensors + preamplifiers
design allows for integration of acoustic sensors into pressure housing of photo sensors
no need for additional mechanical structures
18Kay Graf (ECAP) – VLVnT 09, Athens – October 2009
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Pinger Signals for Reconstruction of Hydrophones and AMs
AMs
Hydros
19Kay Graf (ECAP) – VLVnT 09, Athens – October 2009
signal quality of AMs slightly degraded w.r.t. hydrophones(coupling, ringing of sphere, ...)
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Positioning with AMs
2
30mmσ
• calculate difference of individually reconstructed sensor position• some issues/systematics need to be investigated
20Kay Graf (ECAP) – VLVnT 09, Athens – October 2009
0
1
23
45
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• systematic effects due to orientation of sensors w.r.t. pingers need to be investigated
• for two sensors with distance at 250mm (in a sphere) better than 10° resolution reachable
21Kay Graf (ECAP) – VLVnT 09, Athens – October 2009
Sensors 0 and 2
Heading on AM Storey
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Positioning Option for KM3NeT
AMADEUS-like acoustic sensors have the potential to combine:
• positioning
• investigation of acoustic neutrino detection techniques
• marine science
Acoustic Modules (AMs) allow for an integration of acoustic sensors into Opto-Acoustical Modules (OAMs).
First Measurements in the Lab:
• no significant degradation of performance of acoustic sensors by ANTARES HV base
• noise expected mainly from DC-DC converter
22Kay Graf (ECAP) – VLVnT 09, Athens – October 2009
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Source Reconstruction
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 23
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Source Direction Reconstruction: A Dolphin
• beam forming or time difference algorithms used• uncertainty <1°
(mainly due to binning in the algorithm)
24
Inte
nsity
(au
)
-180 0 180f (°)
0 0.5 1time (ms)
90
0
-90
(°
)
1
0
-1
Am
plit
ude
(a
u)
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009
most probable source direction
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Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 25
Angular Distribution of Marine Sound Sources• direction reconstruction for one storey• all types of transient signals included• origin points horizontal to north• one month of data
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Tracking of a Source
• reconstruction with one storey• all triggered events within 500s displayed
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 26
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Summary
• at UHE neutrinos are the only viable messenger beyond the local universe
• need a >100km2 ∙ 2∙ year detector
•acoustic detection promising candidate
• complementary to optical and radio techniques (hybrid detection)
•AMADEUS in ANTARES: feasibility study for a future acoustic detector
• dedicated array in a detector environment – hybrid detection possible
• successfully operated since 12/2007
• return of experience for future arrays (opto-acoustical?)
Kay Graf (ECAP) – VLVnT 09, Athens – October 2009 27
Funded by: