by nicolas picot-clemente cnrs/cppm, marseille antares experiment status and first results …
TRANSCRIPT
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