byNicolas PICOT-CLEMENTE

CNRS/CPPM, MarseilleANTARES experiment status and first results

Neutrino telescope: Detection principlenmg43Sea floorpnmnmmp, agReconstruction of m trajectory (~ n) from timing and position of PMT hits interactionCherenkov light from m3D PMT array

CPPM, Marseille DSM/IRFU/CEA, Saclay APC Paris IPHC, Strasbourg Univ. de H.-A., Mulhouse IFREMER, Toulon/Brest C.O.M. Marseille LAM, Marseille GeoAzur Villefranche LPC, Clermont Ferrand (new) University/INFN of Bari University/INFN of Bologna University/INFN of Catania LNS Catania University/INFN of Pisa University/INFN of Rome University/INFN of Genova IFIC, Valencia UPV, Valencia NIKHEF, Amsterdam KVI Groningen NIOZ Texel ITEP,Moscow University of Erlangen ISS, Bucarest The ANTARES Collaboration

The ANTARES site & Infrastructure

JunctionBoxInterlink cables40 km toshore 900 PMTs 12 lines + I.L. 25 storeys / line 3 PMTs / storeyThe ANTARES detector

ANTARES Construction MilestonesMarch 2006: First line connected.September 2006: Line 2.January 2007: Lines 3-5.December 2007: 10 Lines on the site.May 2008: Whole detector.

Expected performance (MC Studies)Angular resolution better than 0.3 above a few TeV, limited by: Light scattering + chromatic dispersion in sea water: s ~ 1.0 ns TTS in photomultipliers: s ~ 1.3 ns Electronics + time calibration: s < 0.5 ns OM position reconstruction: s < 10 cm ( s < 0.5 ns) increases with energy Earth opacity above 100 TeV

Detector visibilityMkn 501Mkn 421Mkn 501RX J1713.7-39GX339-4GalacticCentreAMANDA/IceCube (South Pole)ANTARES (43 North)

Background light under sea water

Bioluminescence and K40 desintegration40K40Cage- (b decay)gCherenkovAlso used for in situ time calibrations (see Garabed Halladjian s talk)

Atmospheric muons and neutrinosExpected atmospheric muons and neutrinos.

Atmospheric muonsVertical muon intensity versus depth with data from Line 1.

Atmospheric muonsA muon event with the 12-line detectorHit ElevationHitTimePlenty circle: hit selected by the trigger.Empty square: hit used by the fit.Cross: hit saved in 2.2 ms around the event.

A neutrino candidate

Rate per dayReconstructed data per day compared to Montecarlo with the 5-line detector.168 detected during 139 days with the 5 lines

ANTARES and physics

?Gamma-Ray Bursts What and why ?Dark matterPoint sourcesMagnetic Monopoles

The Gamma Ray Burst

Short pulses (1ms to 100 s) of g-rays (~ 1 MeV)BATSEThe Gamma Ray Burst (GRB)Burst duration2 distinguishable classesVery different signalsBut

Should appeared with extreme conditions during violent and far astrophysics phenomenons (0.03 < z < 6.29). Binary systems.The Gamma Ray Burst (GRB) Short pulses (1ms to 100 s) of g-rays (~ 1 MeV). Collapse of massive star and black hole formation surrounded by an accretion disk., Burst duration2 distinguishable classes

100111011100111011detectorAll data before, during and afterGRBAll dataThe Gamma Ray Burst (GRB)The acquisition system

The Gamma Ray Burst analysisAnalysis for the 5-line detector is ready.Use of a specific trigger, of an improve reconstruction and of some cuts (Nhits, Totampl, qzen,)Excellent signal over noise ratio remaining after analysis ~ 10. With an angular resolution ~ 2.6.

The point-like source search

Sources coming from differentcatalogues (HESS, Magic, ...)In Hadronic models TeV n should be produced in roughly equal numbers to TeV g-rays.VHE ray sources represent prime targets for neutrino telescopes.69 sources selected in ANTARES field of view50 Galactic sources among: Pulsar Wind Nebulae (PWN)Supernovae Remnants (SNRs)g-Ray Binaries....19 extragalactic sources : Quasars, ...Galactic coordinatesPoint-like source search

* Sources closer than the ANTARES angular resolution (0.3 above a few TeV) are considered as a single point-like source. PWN are excluded because generally treated as leptonic emitters (exceptions for Crab & VelaX).Point-like source search

Point-like source sensitivityPoint-like source analysis results for the 5-lines detector will arrive soon !

The dark matter

Dark matter searchWIMP Accretion into the sun Self-annihilationANTARES En MWIMPsSun

Dark matter searchLKPs (Lightest KK Particles), non-baryonic and neutral particles corresponds to the first KK-resonance level of the hypercharge boson B(1)PRELIMINARY

Kaluza-Klein model (KK):All the Standard models fields propagated in extra-dimensions (conventionnal space-time + 1 space dimension with a compactification radius R)Msugra theories:Contains all the known fields of the SM and an extra Higgs doublet, together with the partners needed to form supersymmetric multiplets.The LSP the lightest supersymetric particule, the neutralino (c), is stable and weakly interacting, and is our Dark Matter candidate.

6 fundamental annihilation channels leading to neutrinos.

The magnetic monopoles

Magnetic monopole search Dirac in 1931 : e-M.M.the smallest magnetic charge, called the Dirac charge. tHooft and Polyakov in 1974 : Non perturbative solutions which looks like Dirac M.M. in non-abelian gauge theories.Those solutions appear each time a compact and connected group is broken into a connected sub-group.GnralisationTransition example with the minimal GUT group:MM with charge g=gD, not affected by the second transition.radius ~ 10-28 cmmass ~ 1016 GeV

Cherenkov photons from delta-rays.Direct Cherenkov photons from a MM with g=gD.x 8500Cherenkov photons from a muon.nsea water ~ 1.35Number of photons emitted by a MM with the minimal charge gD, compared to a muon of same velocity :8500 times more !Direct Cherenkov emission > 0.74 :Indirect Cherenkov emission > 0.51 :The energy transferred to electrons is sufficiently important to pull out electrons (d-rays). These can emit Cherenkov light.Magnetic monopole signal in sea water

Magnetic monopole searchAMANDA IIMACROPARKER127127Expecting sensitivity with a C.L. of 90% for the 5-line detector after 127 days of data taking with some preselection cuts (not interesting for slow M.M. with b < 0.75).PRELIMINARY

A new project with an optical follow-up

Neutrino detection with an optical follow-upPrinciple:Neutrinos are used this time as triggers for an optical telescope.Conditions: 2 n from the same direction (< 3) in 15 minutes. 1 H.E. n with the best reconstruction. Two 25 cm telescopes located at Calern (South France) and La Silla (Chile). 1h of optical data taking after the alert.A collaboration with TAROT:Number of expected alert per month: 1 or 2.Implementation of an online analysis program in progress. First alert very soon

Conclusion

OM rates

Atmospheric muonsDowngoing muon eventHit ElevationHitTime

**Simulation de linteraction nNmX Section efficace vs nergie Absorption dans la Terre

Simulation des bruits de fond muons atmosphriques muons induits par n atmosphriques*M. Spurio- ANTARES*****************************************