ANTARES%20neutrino%20telescope%20status%20and%20indirect%20searches%20of%20Dark%20Matter%20%20%20Guillaume%20Lambard%20%20Centre%20de%20Physique%20des%20Particules%20de%20Marseille%20France

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ANTARES neutrino telescope status and indirect
searches of Dark MatterGuillaume
LambardCentre de Physique des Particules de
MarseilleFrance
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Antares collaboration location
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The Detector
SCM
P 250 bars
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A detection storey
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Antares detection principle
WATER
Cerenkov cone
Detector
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FLOOR
µ track
Time local coincidences between OMs and Storeys
-gt Time hits distributions Vs Detection locations
Charged current interaction
?µ
ROCK
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Observable sky by Antares at the latitude of 43
ANTARES galactic coordinates skymap of visibility
Galactic center position
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-180
180
-90
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Antares.com Breaking news
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
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Physical expected performances
E lt10TeV kinematic E gt10TeV the detector

• Angular resolution lt 0.3 (EgtTeV) limited by
• TTS in photomultipliers s 1.4 ns
• Time Calibration s 0.6 ns
• Line positioning s lt 10cm (s lt 0.5 ns)
• Scattering and chromatic dispersion s lt 1.0 ns

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Physical expected performances
For 12 lines
Earth opacity for E gt 100 TeV
Increase with energy
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Reconstruction results
Case of ten lines reconstruction for a down-going
event
m

• T 124.0
• Track projection in phase space (z,t)

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Reconstruction results
Case of ten lines reconstruction for an up-going
event
m

• q 51.9

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Reconstruction results
Hits distribution over zenith and azimuth angles
Discrepancies MC/data Work on the OMs acceptance
in progress
Azimuth angle ? detector topology effect on the
hits distribution At 12 Lines, the detector will
be symmetric and this effect should disappeared
in part
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Reconstruction results
All events
Reconstruted up-going events
Reconstructed Quality factor
Quality cut dertermined after Monte-carlo studies
to discritimate the real up-going events with the
down-going and misreconstructed events
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Dark Matter search perspectives in the Sun
ANTARES
WIMP
?
Accretion into the sun Self-annihilation
Sun
E? ? MWIMPs
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Dark Matter search perspectives in the Sun
Dark Matter indirect detection side
independent-model

• WIMPs traking down into heavy bodies by elastic
  scaterring and gravitational accretion
• Self-annihilations into primary and secondary
  neutrinos
• Interaction neutrinos/matter into the
  source-body
• Neutrinos oscillations from the source to the
  Earth
• Neutrinos/Earth medium charged current
  interactions -gt muons
• Effective Area, neutrinos flux and source
  visibility -gt number of events

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Annihilation rate and channels
WIMPs lose energy through an elastic scaterring
off nucleons into the Sun medium Equilibrium for
Capture rate annihilation rate
? a (1000 GeV / mB(1))-6 tanh2(mB(1)-13/4)

• Considered channels
• Primary neutrinos cc ? nn, dN/dE (1/Mc)², UED
  model
• Secondary neutrinos (Bertone, Servant, Sigl)
  from
• cc ? qq ? p/- ? nm ?? enenmnm,
• heavy quarks decay (before Hadronization) b,
  c, t
• t leptons and doublet of higgs dd
• And WW, ZZ for neutralinos(MSSM, mSugra, etc...)
• Muon flux

(GeV-1.m-2.an-1)
Oscillation over 3 flavors ne/nµ/nt from the Sun
to the Earth
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UED model

• UED model(Universal Extra-Dimensions) Every
  fields of the Standard Model propagate into the
  extra-dimensions (conventional space-time 1
  space dimension with a compactification scale to
  R constraints by the accelerator experiments)
• Conservation of the Kaluza-Klein parity in
  effective 4-dim theory
• KK lightest state ? Dark Matter candidate
• LKPs (Lightest KK Particles), non-baryonic and
  neutral particles corresponds to the first
  KK-resonance level of the hypercharge boson
• B (1) where (Servant-Tait)

• self-annihilation channels

B(1) B(1) ? ff, hh, ?? ? ?, p,
e, e- , ?
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Expected muons from DM self-annihilation
Sun visibility for Antares in zenith angle
Anticipated atmospheric bkg neutrinos per sec.
Upward going part
400GeVltMLKPlt1TeV Relic density r0 0.3
GeV/cm3 vLKP220 km.s-1 sSD10-6pb Compared to
the atmospheric background 5 evts for 3 in cone
aperture around the Sun
Expected muons events from the B(1)
self-annihilations
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Sensitivity of Antares to neutrinos from the
Sun In the mSugra assumptions
(at 12 lines)
PRELIMINARY
Lower limit from the  soft channel 
(cc-gtbb) Upper limit from the  hard
channel (cc-gtWW)
Updates for 5 10 lines configuration in
progress
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Dark Matter annihilations in mini-spikes

• Detection of neutrinos from Dark Matter
  annihilations into the mini-spikes around
  Intermediate Mass Black Holes (IMBHs)
• Mini-spikes -gt bright sources of neutrinos
• Mini-spikes from the reaction of DM mini-halos to
  the formation of IMBHs
• IMBHs model study MIMBHs 105 M?
• Better sentivity and high energy resolution of
  ACTs(HESS, INTEGRAL, CANGAROO,) can be used to
  discriminate mini-spikes from the ordinary
  Astrophysical sources. But the full surveys
  favored the sea neutrino telescopes(Antares
  IceCube).
• The location of Antares and an effective area of
  1km2 appears to be the best for the detection-gt
  Good perpectives for KM3-net

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Mini-spikes ramdom distribution in the milky way
ANTARES galactic coordinates skymap of visibility
Galactic center position
Equatorial coordinates skymap of IMBHs in one
random realization (red diamonds) and 200
realizations (blue diamonds) with a great
concentration around the Galactic Center (yellow
circle)
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Prospects from mini-spikes assumptions
Prospects for detecting Dark Matter with neutrino
telescopes in Intermediate Mass Black Holes
scenarios G. Bertone arXivastro-ph/0603148v2
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Conclusions perspectives
PRELIMINARY
Galactic coordinates skymap of 116 up-going events

• Through a precise time calibration and acoustic
  positioning of the lines, we are able to extract
  
• a full sky map and potentials spikes positions
  into the neutrinos distribution with an
  integrated data taking time gt 300 days (5 10
  lines configurations take into account)
• put limits over the LSP, LKP, etc Dark Matter
  candidates masses by Sun, GC correlations the
  events direction through blind and unblind
  strategies (interesting for signals at low
  statistics)
• Good perpectives from the IMBHs models and
  growths of mini-spikes around. But, difficulty to
  discriminate the neutrinos flux from Dark Matter
  self-annihilations to the classic Astrophysical
  events. Needed a crosscheck with the GRs data.

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BACK UP
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Expected neutrino flux from the Sun

• Neutralino LSP in mSugra theory
• mSugra parameter space through
  m0,m1/2,A0,tan(b),sign(m)

Expected neutrinos flux from the source
Expected neutrinos events
All models studied 0,094 lt Oh² lt 0,129 (WMAP 3yr
constraint) O h² lt 0,094
All models studied 0,094 lt Oh² lt 0,129 (WMAP 3yr
constraint) Better signal
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BackupIn situ calibration quality
Coincidences rates through the 40K decay (40K ?
40Ca e- ?e)
Coincidences between adjacent optical modules
Cerenkov photons produced by relativistic
electrons
40K ? 40Ca e- ? 2?
Adjacent floor coincidences
Integral under the peak muon flux Shape is
sensitive to angular acceptance of optical
modules andangular distribution of muon flux
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BackupLED Beacons Illuminations
Examples and view of in situ calibration by the
LED beacon system in the sea. The mean of these
distributions centered around 0 check the good
quality of the time calibration before the
deployment.
Events
t ( ns)
Events
t ( ns)
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Backup Background noise expected
Muons distribution over zenith angle
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Backup Trigger

• Before to really reconstruct a muon track, there
  are five data processing levels from the data
  taking to the discovering of potential events
• Level 0 (L0) All hits
• Level 1 (L1) local trigger search
• local coinciding hits in a time gate (20 ns) on
  2 PMTs of the same floor
• and/or all hits with charge gt threshold param.
  (2.5 p.e.)
• Level 2 (L2) global trigger search
• Space-time relation between signals due to
  unscattered light from the same muon trajectory
  or bright point
• assuming high relativitic muons, slowest
  possible speed c/n (n1.35). For two hits,
  causality implies

?t time between hits ?x diff. Between PMTs
positions
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Backup Trigger

• Level 2 (L2)
• if the number of correlated hits gt
  minClusterSize parameter(4) ? Cluster
• For example for a 3D Trigger
• Minimum number of hits in the cluster 5
• Minimum number of floors in the cluster 5
• Minimum charge of the largest hits in the
• cluster 0.3 p.e.
• etc
• Level 3 (L3) merging of overlapping events
• each event contains a snapshot of all hits in a
  time window around the cluster
• tmaxCausal 2.2 µs
• All hits within causality condition added
• Level 4 (L4) event building
• All raw hits collected in a snapshot and
  combined into PhysicsEvent with data of
  clusters

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Backup Trigger

• After, all processing levels used into different
  forms of triggers which look for
• 1D time correlated hits in a given direction
  (L0 data in input)
• 3D time correlated hits from any directions
  (L1 data in input)
• MX similar to 1D one local coincidence (1
  L1) to speed up the processing of L0 data
• And the number of L0 or L1 levels for each
  trigger can vary
• At the end, the muon track reconstruction
  strategy can apply to the selected hits

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Backup Reconstrustion Strategy

• Step 1 Linear prefit by ?²-minimization over
  local coincidences and integrated charge of hits
• step 2 M-estimator minimization
• Ai charge, ri time residual, fang angular
  factor, K0.05 (MC simulation)
• step 3 Likelihood-maximization

A likelihood cut is preformed to discriminate the
real up-going events compare to the
down-going muon misreconstructed.
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Backup Neutrinos Effective Area
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Backup Neutrinos cross sections
scc,? from CTEQ coll. Parton Distribution
Functions
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Backup Reconstruction results
Last case with five Lines
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Backup Reconstruction results
run 25685, frame 81559
3D reco. (A. Heijboer)
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Backup Energy reconstruction
Factor 2 or 3 at low energy (ltO(TeV))
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Backup Sun Case

• Systematical analysis of data through an angular
  cut (dominated by the angular resolution at low
  energy) and an common ON/OFF area method. The
  up-going neutrinos events extracting into a 2
  cone around the Sun position
• Likelihood cut

• Sun position computation into the
  topocentric(zenith and azimuth angle) and
  geocentric(declination, right ascention) frames,
  and eventually the apparent diameter to improve
  the cone aperture-gt Common SLALIB library through
  an Antares ROOT Kit analysis dedicated

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Backup Sun Case
Apparent diameter 0.53-gt angular resolution
still dominates Possibility to evaluate an
expected background spectrum in zenith angle from
the atmospheric neutrinos interactions