Status of the ANTARES Neutrino-Telescope Alexander Kappes Physics Institute University Erlangen-Nuremberg for the ANTARES Collaboration WIN´05, 6.–11. June 2005 Delphi, Greece Introduction The ANTARES Detector First Results from Test- Lines Outlook
Status of the ANTARES Neutrino-Telescope. Alexander Kappes Physics Institute University Erlangen-Nuremberg for the ANTARES Collaboration. WIN´05, 6.–11. June 2005 Delphi, Greece. Introduction The ANTARES Detector First Results from Test-Lines Outlook. - PowerPoint PPT Presentation
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Status of the ANTARES Neutrino-Telescope
Alexander KappesPhysics InstituteUniversity Erlangen-Nurembergfor the ANTARES Collaboration
WIN´05, 6.–11. June 2005Delphi, Greece
Introduction The ANTARES Detector First Results from Test-Lines Outlook
6. - 11. June 2005 WIN´05 Delphi, Greece
2Alexander Kappes University Erlangen-Nuremberg
Active Galactic Nuclei
Supernova Remnant (RX J1713.7-3946)
Gamma Ray Burst
Cosmic accelerators
(Bepposax)
Hubble
H.E.S.S.
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Detection of Cosmic Neutrinos
A ! X
Earth used as shield against all other particles
Čerenkov light:
Čerenkov angle: 42o
wave lengths used: 350 – 500 nm
low cross section requires large detector volumes
key reaction: + A ! + X
Detector deployed in deep water / ice to reduce downgoing atmospheric muons
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Physics with Neutrino Telescopes
Searching for point-like neutrino sources
Measurement of diffuse neutrino flux
Search for Dark Matter (WIMPs)
Search for exotic particles:e.g. magnetic monopoles
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Why a Neutrino Telescope in the Mediterranean Sea? Sky coverage complementary to telescopes at South Pole Allows to observe the region of the Galactic Centre
Not seenNot seenMkn 501Mkn 501
Mkn 421Mkn 421
CrabCrab
SS433SS433
Mkn 501Mkn 501
GX339-4GX339-4SS433SS433
CrabCrab
VELAVELA
GalacticGalacticCenterCenter
Not seenNot seen
South Pole Mediterranean Sea
Sources of VHE emission (HESS 2005)
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The ANTARES Collaboration
20 institutions from 20 institutions from 6 European countries6 European countries
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The ANTARES Detector46
0 m
70 m
14.5
m
Str
ing
OpticalModule
JunctionBox
Buoy
Submersible
Cab
le to
Sho
re s
tatio
n
artist´s view(not to scale)
Hostile environment: pressure up to 240 bar sea water (corrosion)
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One of 12 ANTARES Strings
Buoy keeps string vertical
(horizontal displacement < 20 m)
Storey 3 optical modules (45o downwards) electronics in titanium cylinder
Instrumentation components: current profiler (ADCP) sound velocimeter water properties (CSTAR, CT)
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First results from MILOMTiming calibration with LED beacons: Measured relative offset of 3 optical modules on same storey Large light pulses used ) TTS of PMT small
Optical beacon signal
Time (ns)
Am
plit
ud
e
Time difference between optical modules
electronics contribution to resolution around 0.5 ns investigations in progress to separate various contributions
t OM1 – OM0 t OM2 – OM0
=0.75ns =0.68ns
beacon signal
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First results from MILOMAcoustic positioning: Several acoustic transponders installed Currently only results from 1D measurements available
Systematic effects under control on the level of 2 mm.
Time (day)2 4 6 8 10 12 14 16 18 20
96.58
96.59
96.60
96.61
Dis
tan
ce (
m)
distance from transponder (anchor) to receiver (first storey) vs. time
distribution around daily average
8 6 4 2 0 2 4 6 8Distance (mm)
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First Results from MILOM
Compass headings from all three MILOM storeys:
mostly synchronous movement of all storeys
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First results from MILOM
Environmental data:
Water temperature
+ sound velocity
Temperature almost constant at 13.2oC
Water temperature determines sound velocity (at given depth)
Water temperature
Sound velocity
Vel
oci
ty (
m/s
)
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First results from MILOM
Environmental data: Sea current (current profiler)
Most times sea current < 15 cm/s Significant changes of direction over periods from hours to days
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First results from MILOM
MILOM is a big success:
Data readout (waveforms + SPE) is working as expectedand yields ns timing information
In situ timing calibration and acoustic positioning reach expected resolution
All environmental sensors are working well
Continuous data from Slow Control (monitoring of various detector components)
Lots of environmental and PMT data available; intensive studies ongoing
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Line0 deployed to test mechanical structure equipped with autonomous recording devices
water leak sensors sensors connected to electrical and fibre loops
for attenuation measurements recovered in May 2005
Results: no water leaks occurred optical transmission losses at various points on fibres
evidently all losses occur inside electronics container at entry and exit from cylinder
presently under intense investigations
On first prototype strings fibres inside cables were
damaged
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ANTARES: further schedule
First full string (Line1) to be deployed and connected end of 2005
Full detector installed in 2007
From 2006 on: physics analysis !
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The future: KM3NeT
common effort of European telescope groups(ANTARES, NEMO, NESTOR) + associated sciences
aim: build and operate a km3 neutrino telescope in the Mediterranean Sea
complementary to IceCube at the South Pole
expect to get EU funding (10 MEuro) for a design study (total budget 24 MEuro) by beginning of 2006
Technical Design Report early 2009
km3 detectors required to exploit full physics potential of neutrino telescopes
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Conclusions MILOM proved to be a big success
data readout is working as expected in situ timing and position resolution sufficient to reach
angular resolution < 0.3o for neutrinos with E > 10 TeV many more data to analyse
Line0 results mechanical structure water tight and pressure resistant optical losses in fibres currently under
intense investigation
First full string expected to be deployed this year;Full detector in 2007