tev particle astrophysics ii madison, wi, usa august 28 – 31, 2006
DESCRIPTION
TeV Particle Astrophysics II Madison, WI, USA August 28 – 31, 2006. Towards Acoustic Detection of UHE Neutrinos in the Mediterranean Sea – The AMADEUS Project in ANTARES. N.G. Lehtinen et al., Astropart. Phys., 17 (2002), p. 279. Acoustic Detection of UHE Neutrinos. - PowerPoint PPT PresentationTRANSCRIPT
Kay Graf
Physics Institute
University of Erlangen
TeV Particle Astrophysics IIMadison, WI, USA
August 28 – 31, 2006
Towards Acoustic Detection of UHE Neutrinos
in the Mediterranean Sea–
The AMADEUS Project in ANTARES
August 28 – 31, 2006TeV Particle Astrophysics II – Madison
Kay Graf University of Erlangen2
Acoustic Detection of UHE Neutrinosenergy deposition in (hadronic) cascade
) disc-shaped bipolar pressure pulse
N.G. Lehtinen et al., Astropart. Phys., 17 (2002), p. 279
August 28 – 31, 2006TeV Particle Astrophysics II – Madison
Kay Graf University of Erlangen3
AMADEUS: Project and ObjectivesAMADEUS:
ANTARES Modules for Acoustic Detection Under the Sea
equip several storeys of the ANTARES detector with acoustic sensors
• evaluate the feasibility of an acoustic neutrino detector using a dedicated array of sensors
• investigate the acoustic background: noise and signals at different length scales comparable to a future detector
• test hardware/software and signal processing in a realistic surrounding
located in a deep-sea environment) within the framework of the ANTARES experiment
August 28 – 31, 2006TeV Particle Astrophysics II – Madison
Kay Graf University of Erlangen4
Simulations of an Acoustic DetectorT. Karg, PhD Thesis, astro-ph/0608312
(2006)
effective volume and energy threshold strongly dependent
on detection threshold of sensors
) design and test efficient signal processing algorithms
rate of correlated neutrino-like background events is not
known, only random coincidences assumed
) measure with AMADEUS at different length scales
200 acoustic modules in Vinstr. = 1 km3
August 28 – 31, 2006TeV Particle Astrophysics II – Madison
Kay Graf University of Erlangen5
Previous Studies at ANTARES siteautonomous system with acoustic sensors inside Ti-cylinder
on ANTARES test line (2005)
successful data taking for 20 h
but limited capability (electronics noise, vessel)
) test data processing algorithms
anchor of Line0anchor of Line0
August 28 – 31, 2006TeV Particle Astrophysics II – Madison
Kay Graf University of Erlangen6
Previous Studies at ANTARES siteSPY Hydrophone (CPPM Marseille) on MILOM (since 2005)
electronics and software fully working,but not sensitive to background noise (40 dB loss)
) SPY II on next Instrumentation Line
T im e ( m s )
T im e ( m s )
sp ectro g ra m
P in g R x T x ( 5 4 k H z, 1 m s )
A D C PR x T x
storey of MILOMstorey of MILOM
P (
Pa)
f (k
Hz)
time (ms)
time (ms)
August 28 – 31, 2006TeV Particle Astrophysics II – Madison
Kay Graf University of Erlangen7
Instrumentation Line with
3acoustic storeys
(+SPY II) (deployment
foreseen first half 2007)
3 more acoustic storeys in
another line(plans to be
finalized)
AMADEUS at ANTARESANTARES storey
2
m
August 28 – 31, 2006TeV Particle Astrophysics II – Madison
Kay Graf University of Erlangen8
From Optical to Acoustic Storey
or
Concept: • no interference with ANTARES optics • as little design changes as possible
Main changes:• sensors: optical modules to hydrophones or acoustic
modules• off-shore digitization boards: ARS board to acoustic
ADC board• new on-shore PC farm
August 28 – 31, 2006TeV Particle Astrophysics II – Madison
Kay Graf University of Erlangen9
Piezoceramic Sensorsacoustic module:
2 sensors (piezo with preamplifier)
in one glass sphere
hydrophones:2 separate sensors
(commercial or custom)
complementary:use both!
+ water tightness guaranteed+ no design changes needed+ no pressure on components
- alters acoustic signal
+ position can be optimized+ characteristics tuneable+ better directional sensitivity
- assure water tightness
August 28 – 31, 2006TeV Particle Astrophysics II – Madison
Kay Graf University of Erlangen10
Sensor Characteristics – Prototype
self-noise at SS0 level (lowest agitation)(SS0: noise PSD ¸20dB re Pa/Hz1/2 at 30kHz)
commercial hydrophones prototype (18 sensors in production)
sensitivity: measurement andfit from simple piezo model
final version: + 10 – 15 dB
self-noise: after post-amplification and filtering with
ADC board
in air, noisy surrounding
August 28 – 31, 2006TeV Particle Astrophysics II – Madison
Kay Graf University of Erlangen11
Prototype Acoustic ADC Board•analogue part:
•filtering (band pass)
•amplification (1 – 562)
• low noise (O[V/Hz1/2])
•digital part:
•flexible design (FPGA)
•continuous sampling (· 500 kS/sec, 16-bit)
• formatting of data
•communication to shore
• transmission: 1.25 MS/sec per storey
•3 boards per storey, 2 sensors each
• low power ( ¼ 1 W)
August 28 – 31, 2006TeV Particle Astrophysics II – Madison
Kay Graf University of Erlangen12
Performance
•3 (+3) storeys with 18 (36) sensors at 3 length scales ( )
•dynamic range ¼ 3 mPa – 10 Pa (RMS)
•read-out sensors continuously and synchronously at ¸ 200 kS/sec
•data rate 10 (20) MB/sec
•flexible design (sensors, gain, filter)
?
1m
10m
100m
August 28 – 31, 2006TeV Particle Astrophysics II – Madison
Kay Graf University of Erlangen13
Summary and Outlook• 3 ANTARES storeys will be equipped with
acoustic sensors (option for 3 more)• dedicated setup to investigate the
feasibility of an acoustic -detector• currently in prototype and testing phase of
components
Installation of AMADEUS in 2007
if acoustic detection proves feasible) use KM3NeT-infrastructure for acoustics?
(not included in EU design study!)