Presentation is loading. Please wait.

Presentation is loading. Please wait.

Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008.

Similar presentations


Presentation on theme: "Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008."— Presentation transcript:

1 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 ANTARES neutrino telescope status and indirect searches of Dark Matter Guillaume Lambard Centre de Physique des Particules de Marseille France

2 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Antares collaboration & location

3 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 The Detector ~2500 m ~40 km EOC Site/ Seyne-sur-Mer 14.5 m ~350 m instrumented ~100 m Junction box ~70m EMC 12 lines (900 PMTs) 5 sectors/line 5 storeys/sector 3 PMTs/storey storey P ~ 250 bars SCM

4 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 A detection storey

5 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Antares detection principle Charged current interaction µ µ track Čerenkov cone 42° ROCK WATER FLOOR Detector Time local coincidences between OMs and Storeys -> Time hits distributions Vs Detection locations

6 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Observable sky by Antares at the latitude of ~43° Galactic center position ANTARES galactic coordinates skymap of visibility -180°180° 90° -90°

7 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 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

8 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Physical expected performances Angular resolution ~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 : kinematic E >~10TeV : the detector

9 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Physical expected performances Earth opacity for E > 100 TeV Increase with energy For 12 lines

10 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Reconstruction results Case of ten lines reconstruction for a down-going event: Θ = 124.0° Θ = 124.0° Track projection in phase space (z,t) Track projection in phase space (z,t)

11 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Reconstruction results Case of ten lines reconstruction for an up-going event: = 51.9° = 51.9°

12 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Reconstruction results Hits 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…

13 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Reconstruction results Reconstructed Quality factor : Quality cut dertermined after Monte- carlo studies to discritimate the real up-going events with the down-going and misreconstructed events All events Reconstruted up-going events

14 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Dark Matter search perspectives in the Sun WIMP Accretion into the sun Self-annihilation ANTARES E ν M WIMPs Sun

15 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Dark Matter search perspectives in 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:

16 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Annihilation rate and channels WIMPs lose energy through an elastic scaterring off nucleons into the Sun medium Equilibrium for Capture rate = annihilation rate α (1000 GeV / m B(1) ) -6 *tanh 2 (m B(1) -13/4 ) Considered channels : Primary neutrinos, dN/dE = (1/M )², UED model Secondary neutrinos (Bertone, Servant, Sigl) from qq +/- e e, 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

17 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 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 -,

18 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Expected muons from DM self-annihilation Expected muons events from the B (1) self-annihilations 400GeV

19 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 PRELIMINARY (at 12 lines) Sensitivity of Antares to neutrinos from the Sun In 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)

20 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /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 M IMBHs ~ 10 5 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 1km 2 appears to be the best for the detection-> Good perpectives for KM3-net Dark Matter annihilations in mini-spikes

21 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Mini-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

22 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Prospects for detecting Dark Matter with neutrino telescopes in Intermediate Mass Black Holes scenarios – G. Bertone arXiv:astro-ph/ v2 Prospects from mini-spikes assumptions

23 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /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 & perspectives Galactic coordinates skymap of 116 up-going events PRELIMINARY

24 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 BACK UP

25 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Expected neutrino flux from the Sun Neutralino LSP in mSugra theory mSugra parameter space through: m 0,m 1/2,A 0,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 source Expected neutrinos events

26 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Coincidences rates through the 40 K decay ( 40 K 40 Ca + e - + e ): Čerenkov photons produced by relativistic electrons Coincidences between adjacent optical modules Backup:In situ calibration quality 40K 40Ca + e- 2 γ Integral under the peak ~ muon flux Shape is sensitive to angular acceptance of optical modules andangular distribution of muon flux Adjacent floor coincidences :

27 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Backup:LED Beacons Illuminations Events 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.

28 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Backup : Background noise expected… Muons distribution over zenith angle

29 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 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 > 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: Δt : time between hits Δx : diff. Between PMTs positions

30 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Backup : 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

31 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 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…

32 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Backup : Reconstrustion Strategy Step 1 : Linear prefit by χ ²-minimization over local coincidences and integrated charge of hits step 2 : M-estimator minimization A i = charge, r i = time residual, f ang = 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.

33 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Backup : Neutrinos Effective Area

34 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Backup : Neutrinos cross sections σ cc, from CTEQ coll. Parton Distribution Functions

35 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Backup : Reconstruction results Last case with five Lines:

36 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Backup : Reconstruction results run 25685, frame D reco. (A. Heijboer)

37 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Backup : Energy reconstruction Factor 2 or 3 at low energy (< (TeV))

38 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 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-> Common SLALIB library through an Antares ROOT Kit analysis dedicated

39 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology /03/2008 Backup : 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


Download ppt "Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008 Guillaume Lambard - XLIIIrd Rencontre de Moriond – Cosmology 2008 - 15-22/03/2008."

Similar presentations


Ads by Google