results from the antares neutrino telescope
DESCRIPTION
Results from the ANTARES neutrino telescope. G. Giacomelli University of Bologna and INFN Venezia , 27/4/ 2011. Introduction. astronomy ANTARES. Optical detection. Infrastructure Downgoing muons Preliminary n m data Exotica (Fast MMs, Nuclearites,…) Earth-Sea Science - PowerPoint PPT PresentationTRANSCRIPT
ANTARES Results-Venezia 20111
1. Introduction. astronomy
2. ANTARES. Optical detection.
Infrastructure
3. Downgoing muons
4. Preliminary data
5. Exotica (Fast MMs, Nuclearites,…)
6. Earth-Sea Science
7. Conclusions. Outlook
G. GiacomelliUniversity of Bologna and INFNVenezia, 27/4/ 2011
Results from the ANTARES neutrino telescope
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• High energy neutrino astrophysics:Galactic: SN, SNRs, -quasars, molecular clouds, ...
Extra-Galactic: AGNs, GRBs, dark-GRBs, GZK, ....
• Searches for New Physics: Dark matter (Sun, GC), Magnetic Monopoles, ??
• Earth-Sea Science: Oceanography, sea biology, seismology, environmental monitoring
1. Introduction Science with Deep Sea Neutrino Telescopes
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n
p
Neutrino Astronomy
• Advantages w.r.t. other messengers - -Photons: interact with CMB and matter
–Protons: interact with CMB and are deflected by magnetic fields–Neutrons: are not stable
• Drawback: large detectors (~GTon) are needed.
photon
Sky Observable by HE Neutrino Telescopes
Mkn 501
Mkn 421
CRAB
SS433
Mkn 501
RX J1713.7-39
GX339-4SS433
CRAB
VELA
GalacticCentre
AMANDA/IceCube (South Pole)AMANDA/IceCube (South Pole) ANTARES/KM3 (43° NorthANTARES/KM3 (43° North))
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2. ANTARES Site & Infrastructure
Shore Station
IFREMER Toulon Centre
FOSELEV Marine
-2475
m
40 km submarine cable
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č
43°
interaction
ANTARESOptical detection of
Se
ctor
LCM
LCM
LCM
MLCM
LCM
Buoy
SCM
448
m
Storey
3 PMTs
1 MB per PMT
2 ARS
SeabedJunction
box
2.5
km
40 km cable
to shore
14.5
m
Acoustic Positioning
Storey 1Storey 8Storey 14Storey 20Storey 25
Radial displacementPrecision ~ few cms
Measure every 2 min:
Distance line bases to 5 storeys/line
and also storeyheadings and tilts
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reconstructed up-going neutrino:
detected in 6/12 detector lines:
Two Events
reconstructed down-going muon: detected in all 12
detector lines:
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Example: Neutrino candidate
height
time
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height
time
Example of a muon bundle
3. Downgoing muons Depth Intensity Relation from Zenith Distribution
Zenith angle distribution of muon flux at 2000 mAstropart. Phys. 34 (2010) 179
2,5km6km
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Moon Shadow
Search for deficit of downgoing muons
In the direction of the moon (diameter 0.5 degrees)
Verification of the absolute pointing of
the telescope
Preliminary:Live time 295 days:2.5 sigma effect
preliminary
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4. Preliminary data for Upgoing Neutrinos Angular Resolution 2007+2008 analyses:
Angular resolution ~ 0.5°0.4° (ΔΘ < 1° , in 75% of cases)
- Integrated over all energies (E-2
flux)- Half of data only 5 lines
Full 12 line detector
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Sky MapSelection optimized for Model Discover Potential (Λ >-5.4):
(Live time 295 days)
Most significant cluster located at: ra=134.6°, δ=13.4°(post-trial probability to be background 2.4%)
galactic coordinates
2190 selected eventsvisibility
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Point Source Limits
Quoted for E-2 flux
ANTARES-best limits in the Southern sky
More data (2009-2010)on tape
Expect further improvement
energy estimator included
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High Energy Diffuse flux
“Search for a diffuse flux of high-energy νμ with the ANTARES telescope” Phys. Lett. B696 (2011) 16-22.
E2(E)90%= 5.3×10-8 GeV cm-2 s-1 sr-1
20 TeV<E<2.5 PeV
ANTARES Results-Venezia 2011
5. Exotica (preliminary)Fast Intermediate Mass Magnetic Monopoles
• Required in many models of spontaneous
symmetry breaking Upgoing masses less than ~1014 GeV
High photon yield (8.5x103 times μ) Cherenkov threshold >0.74 Delta rays for ≥ 0.5Track reconstruction with free
MM-Cherenkov
muon
MM-delta rays
Monopole
muon
neutrino
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6. Earth-Sea Science Seismograph: Japan Earthquake
In laboratory
Deployment
Buried at site
40 20 0-20-40
AMADEUS: Acoustic Detection of Neutrinos
neutrino
Acoustic Pressure Waves
Hydrophone Array
Cascade
2 min
Bursts: bioluminescence fromMacroscopic organisms
Biocamera
40K
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• The 12 line ANTARES detector is taking data, also with several instruments for Earth Sea Sciences studies.
• The collaboration has shown capable response for solving
technical difficulties (ex.: the breaking of the connecting cable)
•Compared to AMANDA-IceCube, ANTARES completes the coverage of the neutrino sky, with an angular resolution of 0.5°
•First analyses of the downgoing muons allowed calibrations and measurements of the flux; comparison with MC with 30% sis err
•First analyses of neutrinos with 5-12 lines for data taken in
2007-2008 allowed a first search for cosmic point-like sources.
•A search was made for a diffuse flux of H.E. muon neutrinos
•ANTARES sensitivity for point sources is comparable to AMANDA
•First tentative results in Earth and Sea Sciences
•The technical success paves the way to KM3NeT in the Mediterranean
7. Conclusions - Outlook