guillaume lambard - xliiird rencontre de moriond – cosmology 2008 - 15-22/03/2008 guillaume...
Post on 27-Mar-2015
215 Views
Preview:
TRANSCRIPT
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
ANTARES neutrino telescope status andANTARES neutrino telescope status and indirect searches of Dark Matter indirect searches of Dark Matter
Guillaume LambardGuillaume Lambard
Centre de Physique des Particules de MarseilleCentre de Physique des Particules de MarseilleFranceFrance
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Antares collaboration & locationAntares collaboration & location
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
The DetectorThe Detector
~2500 m
~40 km EOC Site/Seyne-sur-Mer
14.5 m
~350 minstrumented
~100 mJunction box
~70m
EMC
12 lines (900 PMTs)5 sectors/line5 storeys/sector3 PMTs/storey
storey
P ~ 250 barsSCM
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
A detection storeyA detection storey
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Antares detection principleAntares detection principle
Charged current interactionµ
µ track
Čerenkov cone
42°
ROCK
WATER
FLOOR
Detector
Time local coincidences between OMs and Storeys -> Time hits distributions Vs Detection locations
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Observable sky by Antares Observable sky by Antares at the latitude of ~43°at the latitude of ~43°
Galactic center position
ANTARES galactic coordinates skymap of visibility
-180° 180°
90°
-90°
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Antares.com : Breaking newsAntares.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
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Physical expected performancesPhysical expected performances
Angular resolution < 0.3° (E>~TeV) limited by:
• TTS in photomultipliers : σ ~ 1.4 ns
• Time Calibration : σ ~ 0.6 ns
• Line positioning : σ < 10cm (σ < 0.5 ns)
• Scattering and chromatic dispersion : σ < 1.0 ns
E <~10TeV : kinematicE >~10TeV : the detector
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Physical expected performancesPhysical expected performances
Earth opacity for E > 100 TeV
Increase with energy
For 12 lines
dlEN
AEffAeENEA
)()()(),(
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Reconstruction resultsReconstruction results
Case of ten lines reconstruction for a down-going event:
ΘΘ = 124.0°= 124.0° Track projection Track projection
in phase space in phase space (z,t)(z,t)
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Reconstruction resultsReconstruction results
Case of ten lines reconstruction for an up-going event:
= 51.9°= 51.9°
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Reconstruction resultsReconstruction resultsHits distribution over zenith and azimuth angles
Azimuth angle detector
topology effect on the hits distribution
At 12 Lines, the detector will be symmetric and this effect should disappeared in part
Discrepancies MC/data
Work on the OMs acceptance in progress…
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Reconstruction resultsReconstruction results
Reconstructed Quality factor :
)1(1.0)log(
SolutionsDOF
NN
L Quality cut dertermined after Quality cut dertermined after Monte-carlo studies to discritimate Monte-carlo studies to discritimate the real up-going events with the the real up-going events with the down-going and misreconstructed down-going and misreconstructed eventsevents
All eventsAll events
ReconstrutReconstruted up-going ed up-going eventsevents
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Dark Matter search perspectivesDark Matter search perspectives
in the Sunin the Sun
WIMPWIMP
Accretion into the sunAccretion into the sun
Self-annihilationSelf-annihilation
ANTARESANTARES
EEνν M MWIMPsWIMPsSunSun
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Dark Matter search perspectives Dark Matter search perspectives
in the Sunin the Sun
● 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 -> muons
● Effective Area, neutrinos flux and source visibility -> number of events
Dark Matter indirect detection side – independent-model:
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Annihilation rate and channelsAnnihilation rate and channels
WIMPs lose energy through an elastic scaterring off nucleons into the Sun mediumEquilibrium for Capture rate = annihilation rate
α (1000 GeV / mB(1))-6 *tanh2(mB(1)
-13/4)Considered channels :➢ Primary neutrinos → , dN/dE = (1/M)², UED model➢ Secondary neutrinos (Bertone, Servant, Sigl) from
➢ → qq → +/- → → ee,
➢ heavy quarks decay (before Hadronization) : b, c, t
➢ leptons and doublet of higgs *
➢ And WW, ZZ for neutralinos(MSSM, mSugra, etc...)
➢ Muon flux:
(GeV-1.m-2.an-
1)Oscillation over 3 flavors from the Sun to the Earth
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
UED modelUED 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- ,
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Expected muons from DM self-annihilation Expected muons from DM self-annihilation
Expected muons events from the BExpected muons events from the B(1)(1) self- self-annihilationsannihilations
400GeV<MLKP<1TeV
Relic density 0 = 0.3 GeV/cm3
vLKP~220 km.s-1
SD~10-6pb
Compared to the atmospheric background ~5 evts for 3° in cone aperture around the Sun
Sun visibility for Antares in zenith angleSun visibility for Antares in zenith angle
Upward going part
Anticipated atmospheric bkg neutrinos per sec.Anticipated atmospheric bkg neutrinos per sec.
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
PRELIMINAR
Y
(at 12 lines)
Sensitivity of Antares to neutrinos from the Sensitivity of Antares to neutrinos from the SunSun
In the mSugra assumptionsIn the mSugra assumptions
Updates for 5 & 10 lines configuration in progress…
Lower limit from the « soft channel » (->bb)
Upper limit from the « hard channel »(->WW)
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
•Detection of neutrinos from Dark Matter annihilations into the mini-spikes around Intermediate Mass Black Holes (IMBHs)
•Mini-spikes -> 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-> Good perpectives for KM3-net
Dark Matter annihilations in mini-spikesDark Matter annihilations in mini-spikes
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Mini-spikes ramdom distribution in the milky wayMini-spikes ramdom distribution in the milky way
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)
Galactic center position
ANTARES galactic coordinates skymap of visibility
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Prospects for detecting Dark Matter with neutrino telescopes inIntermediate Mass Black Holes scenarios – G. Bertone arXiv:astro-ph/0603148v2
Prospects from mini-spikes assumptionsProspects from mini-spikes assumptions
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
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 > 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.
Conclusions & perspectivesConclusions & perspectives
Galactic coordinates skymap of 116 up-going events
PRELIMINARY
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
BACK UPBACK UP
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Expected neutrino flux from the Expected neutrino flux from the SunSun
• Neutralino LSP in mSugra theory
• mSugra parameter space through: m0,m1/2,A0,tan(),sign()
All models studied
0,094 < Ωh² < 0,129 (WMAP 3yr constraint)
Ω h² < 0,094
All models studied
0,094 < Ωh² < 0,129 (WMAP 3yr constraint)
Better signal
Expected neutrinos flux from the sourceExpected neutrinos flux from the source Expected neutrinos eventsExpected neutrinos events
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Coincidences rates through the 40K decay (40K 40Ca + e- + e):
Čerenkov photons Čerenkov photons produced by produced by relativistic relativistic electronselectrons
Coincidences between adjacent optical modules
Backup:In situBackup:In situ calibration quality calibration quality
40K 40Ca + e- 2γ
Integral under the peak ~ muon flux
Shape is sensitive to angular acceptance of optical modules andangular distribution of muon flux
Adjacent floor coincidences :
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup:LED Beacons IlluminationsBackup:LED Beacons Illuminations
Events
Events
t ( ns)
t ( ns)
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.
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup : Background noise Backup : Background noise expected…expected…Muons distribution over zenith
angle
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup : TriggerBackup : 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 > 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 (n~1.35). For two hits, causality implies:
xc
nt
Δt : time between hits
Δx : diff. Between PMTs positions
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup : TriggerBackup : Trigger
• Level 2 (L2) :
• if the number of correlated hits > “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
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup : TriggerBackup : 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…
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup : Reconstrustion StrategyBackup : Reconstrustion Strategy
• Step 1 : Linear prefit by χ²-minimization over local coincidences and integrated charge of hits
• step 2 : M-estimator minimization
Ai = charge, ri = time residual, fang = angular factor, K=0.05 (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.
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup : Neutrinos Effective AreaBackup : Neutrinos Effective Area
dlEN
AEffAeENEA
)(
)()(),(
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup : Neutrinos cross sectionsBackup : Neutrinos cross sections
σσcc,cc, from CTEQ coll. Parton Distribution from CTEQ coll. Parton Distribution FunctionsFunctions
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup : Reconstruction resultsBackup : Reconstruction resultsLast case with five Lines:
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup : Reconstruction resultsBackup : Reconstruction resultsrun 25685, frame 81559
3D reco.
(A. Heijboer)
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup : Energy reconstructionBackup : Energy reconstruction
Factor 2 or 3 at low energy (<(TeV))
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup : Sun CaseBackup : 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-> Common SLALIB library through an Antares ROOT Kit analysis dedicated
Guillaume Lambard Guillaume Lambard - - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008
Backup : Sun CaseBackup : Sun Case
Apparent diameter ~0.53°-> angular resolution still dominates
Possibility to evaluate an expected background spectrum in zenith angle from the atmospheric neutrinos interactions
top related