Exotic Physics searches in ANTARES

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Exotic Physics searches in ANTARES
Workshop on Exotic Physics with Neutrino
Telescopes Uppsala, September 20-22, 2006
Ersilio Castorina Pisa University and INFN on
behalf of the ANTARES Collaboration
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Outline

• Current status of ANTARES
• MC simulation of ? Dark Matter from the Sun
• Ongoing studies (preliminary only)
• early results for ? from the Earth
• first estimate of slow Magnetic Monopoles

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ANTARES

• Astronomy with a Neutrino Telescope and Abyss
  environmental RESearch
• http//antares.in2p3.fr
• Project to build an
• undersea neutrino telescope
• in the Mediterranean Sea

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ANTARES collaboration
Erlangen
NIKHEF Amsterdam, Groningen
ITEP Moscow
IFREMER, Brest DAPNIA, Saclay IReS,
Strasbourg Mulhouse CPPM , Marseille IFREMER,Toulo
n COM, Marseille OCA, Nice
Genova
Bologna
Bari
IFIC Valencia
Roma
Pisa
Catania
LNS
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ANTARES Site
The detector will be located at 2400 m depth, 40
km off the Toulon (France) coast (42º50N,
6º10E) .
The shore station is at La Seyne sur Mer,
40 km NW of the ANTARES site.
Institute Michel Pacha (La Seyne sur Mer)
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Detector Design and Construction Status
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Detector Geometry
12 lines (900 PMTs) 25 storeys / line 3
PMTs/storey
Depth 2400 m
40 km to shore
storey
14.5 m
350 m
100 m
Junction box
70 m
Interconnections
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Neutrino Detection
gc
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2400 m depth
m
Cherenkov light from m induced by n interaction
detected by 3D PMT array Time position of hits
allow the reconstruction of the m ( n)
trajectory
nm
CC interaction
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Basic Dector Element the storey
Optical Beacon for timing calibration
Optical Module 17 glass sphere 10 PMT Ham.
R7081-20 in a cage for magnetic shielding
Local Control Module electronics boards for
readout of PMT signal and data acquisition (plus
calibration equipment)
Hydrophone RX for acoustic positioning
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Construction Status

• Apr 2005 Mini Instrumentation Line
  with OMs (MILOM)

• Mar 2006 Line 1, first complete detector
  line

• 2006 Line 2, deployed in July, to be
  connected TODAY !

• 2006 - 2007 installation of remaining 10
  lines

• 2008 Physics with full detector!

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A Selection of Results Time Calibration

• The timing calibration systems of ANTARES allow
• 100 ns in absolute timing
• 1 ns in relative timing (between OMs)

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A Selection of Results a downgoing m
ANTARES preliminary

• Triggered hits
• Hits used in fit
• Snapshot hits

m
q 172o P(c2,ndf) 0.94
Hit altitude (relative to mid detector) m
Hit time ns
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Searches for Neutralino DMin ANTARES
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ANTARES Science goals

• Neutrinos from point-like diffuse flux sources
• Pulsars
• Young SN Remnants (up to 100 ev/year/km2 )
• Microquasars (SS433 up to 250 ev/year/km2)
• AGN (steady)
• Gamma Ray Bursts (transient 1-100 s)

oceanography, biology, seismology

• Exotic Physics
• Neutrinos from c annihilation in the Sun, the
  Earth and the Galactic Centre
• Magnetic monopoles

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From c down to n
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How many neutrinos ?

• The flux is the sum over the
• possible production channels

The event rate is given by the ?s!
The flux of muons that reach the detector is
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Effective Area for SunGC
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mSUGRA Predictions Sensitivity

• Less constrained models are
• currently under investigation
• Improvements of low E reco will
• affect (i.e. lower) the sensitivity

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Annihilation in the Earth work in progress
mSUGRA flux predictions are extremely low !
Evaluate just the sensitivity (a general MSSM
model could perhaps produce much more neutrinos!)
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Searches for Magnetic Monopolesin ANTARES
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Detection of Magnetic Monopoles

• Monopoles are predicted by Grand Unified Theories

• They can be studied through their interaction
  with matter
• Ionization energy loss
• Radiative energy loss
• Catalysis of proton decay

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Detection of Magnetic Monopoles

• MM produce direct and d-ray induced Cherenkov
  light
• (a tiny but easily detectable fraction of the
  ionization energy loss!)

• Direct Cherenkov emission (bth0.74 in sea water)
• A monopole with gD and b1 emits about 3?106
  photons
• between 300 and 600 nm per cm path length

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Detection of Magnetic Monopoles

• d-ray emission

• Direct d-ray Cherenkov radiation

Kinetic Energy spectrum of d-rays
Cherenkov Threshold for e- in water Tth 0.25 MeV
(Ph.D. Thesis by B. van Rens, NIKHEF)
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Upper limit on Monopole flux below the Cherenkov
limit
Simulation dedicated Trigger Analysis
(Ph.D. Thesis by B. van Rens, NIKHEF)
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Conclusions Outlook
ANTARES has started data acquisition with the
first full line Complete detector by the end of
2007
Thanks and stay tuned!
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Expected Detector performances
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Point-like sources sky visibility
The ANTARES detector will observe 3.5? sr (0.5?
sr overlap with AMANDA). ANTARES will see the
southern sky, AMANDA the northern sky. The
Galactic Centre is observable 67 of the day.
Young Supernova Remnants locations from the Green
catalogue.
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Angular resolution
qmn
mrec
E n lt 10 TeV ? ?-? angle dominated by
kinematic E n gt 10 TeV ? pointing accuracy n
0.2º

ntrue
Reconstruction resolution limited only by
phototube TTS and light diffusion in water
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Point-like sources expected sensitivity A.
Heijboer et al, Point source searches with the
ANTARES neutrino telescope, ICRC 2003
southern sky
northern sky
AMANDA B-10 130 days Engt10 GeV, angular
resolution about 3.9 deg ApJ 583 (2003) MACRO
1388 events in 6 yrs. ltEmgt gt 1.5 GeV, angular
resolution about 0.5 deg SK ICRC2003. 2369
upward-going stopping and through-going muons in
4.6 yr, ltEmgt gt 3 GeV, angular resolution of
about 2.
90 c.l. Muon flux limits (cm-2 s-1)
E-2 neutrino spectrum
AMANDAII sensitivity 2004 197 days (2000)
ANTARES sensitivity 1 yr
After 1 year, Antares can improve limit for
Southern hemisphere or discover something !
Declination (degrees)
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Diffuse Fluxes for nm limits
Sensitivity to diffuse fluxes i. e. integrating
over the full angular acceptance of the detector
Energy resolution allows to set a limit of 810-8
GeV cm-2 s-1 sr-1 after 1 year
Experimental Limits are for E-2 spectra
MACRO
AMANDA UHE
AMANDA
AMANDAII
ICECUBE