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

ANTARES Results-Venezia 20112

• 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

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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