By Nicolas PICOT-CLEMENTE CNRS/CPPM, Marseille ANTARES experiment status and first results …

byNicolas PICOT-CLEMENTE

CNRS/CPPM, Marseille

ANTARES experiment status and first

results …

Neutrino telescope: Detection principle

č

43°Sea floor

p

p,

Reconstruction of trajectory (~ ) from timing and position of PMT hits

interaction

Cherenkov light from

3D PMTarray

CPPM, Marseille CPPM, Marseille DSM/IRFU/CEA, Saclay DSM/IRFU/CEA, Saclay APC ParisAPC Paris IPHC, StrasbourgIPHC, Strasbourg Univ. de H.-A., MulhouseUniv. de H.-A., Mulhouse IFREMER, Toulon/BrestIFREMER, Toulon/Brest C.O.M. MarseilleC.O.M. Marseille LAM, MarseilleLAM, Marseille GeoAzur VillefrancheGeoAzur Villefranche LPC, Clermont Ferrand (new)LPC, Clermont Ferrand (new)

University/INFN of Bari University/INFN of Bari University/INFN of Bologna University/INFN of Bologna University/INFN of Catania University/INFN of Catania LNS – CataniaLNS – Catania University/INFN of PisaUniversity/INFN of Pisa University/INFN of Rome University/INFN of Rome University/INFN of Genova University/INFN of Genova

IFIC, ValenciaIFIC, Valencia UPV, Valencia UPV, Valencia

NIKHEF, Amsterdam NIKHEF, Amsterdam KVI GroningenKVI Groningen NIOZ TexelNIOZ Texel

ITEP,MoscowITEP,Moscow

University of University of Erlangen Erlangen

ISS, BucarestISS, Bucarest

The ANTARES Collaboration

The ANTARES site & Infrastructure

Shore Station

70 m70 m

4450 m50 m

JunctionJunctionBoxBox

Interlink cablesInterlink cables

40 km to40 km toshoreshore

2500m2500m• 900 PMTs • 12 lines + I.L.• 25 storeys / line• 3 PMTs / storey

The ANTARES detector

ANTARES Construction Milestones

March 2006: First line connected.

September 2006: Line 2.

January 2007: Lines 3-5.

December 2007: 10 Lines on the site.

May 2008: Whole detector.

Eff

ectiv

e ar

ea f

or

[m

2 ]Expected performance (MC Studies)

Angular resolution better than 0.3° above a few TeV, limited by: Light scattering + chromatic dispersion in sea water: ~ 1.0 ns TTS in photomultipliers: ~ 1.3 ns Electronics + time calibration: < 0.5 ns OM position reconstruction: < 10 cm (↔ < 0.5 ns)

• increases with energy

• Earth opacity above 100 TeV

dominated by reconstruction

rec− true

rec− dominated

by kinematics

Detector visibility

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 (43° North)ANTARES (43° North)

Background light under sea water …

Bioluminescence and K40 desintegration

March 2006 – May 2008

40K

40Ca

e- ( decay)

Cherenkov

e4020

4019 eCaK

Also used for in situ time calibrations (see Garabed Halladjian ’s talk)

Atmospheric muons and neutrinos

µp

p

Expected atmospheric muons and neutrinos.

Atmospheric muons

Line 1 - 2006 dataLine 1 - 2006 data Line 1 - 2006 dataLine 1 - 2006 data

Vertical muon intensity versus depth with data from Line 1.

Atmospheric muons

A muon event with the 12-line detector

Hit

Ele

vatio

n

HitTime

Plenty circle:

hit selected by the trigger.

Empty square:

hit used by the fit.

Cross:

hit saved in 2.2 s around the event.

A neutrino candidate

Rate per day

Reconstructed 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 matter

Point sources

Magnetic Monopoles

e-

M.M.

The Gamma Ray Burst

Count

rate

in u

nit

of

10

00 c

ounts

s-

1

Total emitted energy: 1053 ergs

Short pulses (1ms to 100 s) of -rays (~ 1 MeV)

BATSE

The Gamma Ray Burst (GRB)

Burst duration

2 distinguishable classes

Very different signals

But

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 -rays (~ 1 MeV).

• Collapse of massive star and black hole formation surrounded by an accretion disk.

If time and position

coïncidences , Very clear signal, with low background in ANTARES

, … Burst duration

2 distinguishable classes

100111011

100111011

location of GRB

detector

All data before, during and after

GRB

alert

save

analysis

All data

The Gamma Ray Burst (GRB)

The acquisition system

The Gamma Ray Burst analysis

Analysis for the 5-line detector is ready.

Use of a specific trigger, of an improve reconstruction and of some cuts (Nhits, Totampl, zen,…)

Prompt GRB range

Angular resolution ~ 2.6°

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 Hadronic models TeV should be produced in roughly equal numbers to TeV -rays.

VHE ray sources represent prime targets for neutrino telescopes.

69 sources selected in

ANTARES field of view

69 sources selected in

ANTARES field of view

50 Galactic sources among: •Pulsar Wind Nebulae (PWN)•Supernovae Remnants (SNRs)•-Ray Binaries....

19 extragalactic sources :• Quasars,• ...

Galactic coordinates

Point-like source search

25

Sources closer than the ANTARES angular resolution (0.3º 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

Added selection criteria have been taken into account for the 5Line data analysis:

Find correlations with those neutrinos

Point-like source sensitivity

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

The dark matter

Dark matter search

WIMPWIMP

• Accretion into the sunAccretion into the sun• Self-annihilationSelf-annihilation

ANTARESANTARES

• EE M MWIMPsWIMPs

SunSun

Dark matter search

Kaluza-Klein model (KK):All the Standard model’s 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 (), is stable and weakly interacting, and is our Dark Matter candidate.

6 fundamental annihilation channels leading to neutrinos.

Self annihilation channel( avec UED: B(1)) :

B(1) B(1) ff, hh*, , p, p, e+, e- ,

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

PRELIMINARY

The magnetic monopoles

Magnetic monopole search

Dirac in 1931 :

e-

M.M.

the smallest magnetic charge, called the Dirac charge.

t’Hooft 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.

Généralisation

Transition example with the minimal GUT group:

MM with charge g=gD, not affected by the second transition.

radius ~ 10-28 cm mass ~ 1016 GeV

Cherenkov photons from delta-rays.

Direct Cherenkov photons from a MM with g=gD.

x 8500

Cherenkov photons from a muon.

nsea water ~ 1.35

Number 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 (-rays). These can emit Cherenkov light.

Magnetic monopole signal in sea water

Magnetic monopole search

AMANDA II

MACRO

PARKER

127

127

Expecting 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 ).

PRELIMINARY

A new project with an optical follow-up

Neutrino detection with an optical follow-up

Principle:

Neutrinos are used this time as triggers for an optical telescope.

Conditions: • 2 from the same direction (< 3°) in 15 minutes.

• 1 H.E. 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