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Status of the ANTARES Neutrino Telescope PowerPoint Presentation
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Status of the ANTARES Neutrino Telescope

Status of the ANTARES Neutrino Telescope

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Status of the ANTARES Neutrino Telescope

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  1. research goals • detector setup • selected results • summary Stéphanie ESCOFFIER CPPM Marseille, France on behalf of the ANTARES Collaboration Status of the ANTARES Neutrino Telescope

  2. Neutrino astronomy • Cosmic sources of neutrinos • micro quasars: X-ray binaries • supernova remnants and shock acceleration • Active Galactic Nuclei • Gamma Ray Bursts • Intriguing science questions: • astrophysical acceleration mechanism ? • origin of cosmic rays ? • dark matter ? • other exotic physics (magnetic monopoles) ?

  3. 7 COUNTRIES 28 INSTITUTES ~ 150 SCIENTISTS AND ENGINEERS The ANTARES Collaboration • University of Erlangen • Bamberg Observatory • University/INFN of Bari • University/INFN of Bologna • University/INFN of Catania • LNS – Catania • University/INFN of Pisa • University/INFN of Rome • University/INFN of Genova • NIKHEF (Amsterdam) • KVI (Groningen) • NIOZ Texel • ITEP, Moscow • Moscow State Univ • CPPM, Marseille • DSM/IRFU/CEA, Saclay • APC, Paris • LPC, Clermont-Ferrand • IPHC (IReS), Strasbourg • Univ. de H.-A., Mulhouse • IFREMER, Toulon/Brest • C.O.M. Marseille • LAM, Marseille • GeoAzur Villefranche IFIC, Valencia UPV, Valencia UPC, Barcelona ISS, Bucarest

  4. 14.5 m ~60 m The ANTARES detector Buoy • 12 lines of 75 PMTs • 25 storeys / line • 3 PMTs / storey • ~900 PMTs Storey 350 m 40 km to shore Junction Box Submarine links Completed in May 2008

  5. The background • (Particle) Physics background • cosmic rays (atmospheric μ and ν) PMT counting rates • Optical background • constant 40K (~40 kHz) Cherenkov light • bioluminescence of micro-organisms e- • bursts from macro-organisms 40K beta decay 2 min 40Ca 40K is used to check the time calibration of the detector

  6. The background • (Particle) Physics background • cosmic rays (atmospheric μ and ν) PMT counting rates • Optical background • constant 40K (~40 kHz) • bioluminescence of micro-organisms • bursts from macro-organisms 2 min strongly correlated to sea currents

  7. The background • (Particle) Physics background • cosmic rays (atmospheric μ and ν) PMT counting rates • Optical background • constant 40K (~40 kHz) • bioluminescence of micro-organisms • bursts from macro-organisms 2 min special event in 2006: ANTARES Coll., Deep-Sea Res. I 58 (2011) 875.

  8. The online/precise tracking • Online tracking • fast, to discriminate atmospheric muons • from neutrinos • No detailed calibration/ no real time detector • positioning needed • Angular resolution: Δθ 3o Astropart.Phys. 34 (2011) 652 • The precise tracking • detailed real-time positioning of the detector • detailed PMTs charge/time calibration • detailed systematic knowledge of the apparatus • (OMs angular acceptance, etc.) • Angular resolution: up to Δθ0.2o arXiv 0908.0816

  9. Event display: a neutrino candidate online tracking height Example of a reconstructed up-going muon (i.e. a neutrino candidate) detected in 6/12 detector lines: time

  10. Selected results atmospheric muon flux atmospheric neutrinos point sources  see talk by Juan Pablo Gomez diffuse νμ flux magnetic monopoles dark matter  see talk by Juande Zornoza

  11. Atmospheric muons online tracking Data MC (corsika + qgsjet) Systematics on MC corsika + qgsjet (poly) corsika + sibyll mupage Zenith angle distribution of reconstructed tracks from atmospheric muons with a 5 line detector. Astropart.Phys. 34 (2010) 179. • systematic error due to +/- 10% on absorption length = +25%/-20%; • syst. err. due to -15% on PMT efficiency (QE, eff. area etc) = -15%; • syst. err. due to cutoff in angular accept. = +20%/-15%; • total systematic uncertainty +/- 30%.  Within systematic uncertainties the measurements cannot distinguish between the models considered Systematic uncertainties: +30% primary flux; +25% hadronic interaction model

  12. 2,5km 6km Muon depth-intensity relation Astropart.Phys. 34 (2010) 179.  Results are in agreement, within the systematic uncertainties, with the theoretical predictions and previous measurements

  13. Atmospheric neutrinos online tracking data set: 2007-2008 data taken with 5 lines (2007) and 9, 10, and 12 lines (2008) up-going down-going 341 days detector live time, single- and multi-line fit 1062  cand. • good agreement with Monte Carlo • atmospheric neutrinos: • 916 (30% syst. error) • atmospheric muons: • 40 (50% syst. error) elevation angle  1062 neutrino candidates:  3.1  candidates/day

  14. Badly reconstructed Well reconstructed Search for point-like  sources arXiv:1108.0292v1 [astro-ph.HE] precise tracking data set: 2007-2008 data taken with 5 lines (2007) and 9, 10, and 12 lines (2008) uncertainties in angle reconstruction: median: 0.5  0.1O 12-line data: 0.4  0.1O absolute orientation: 0.1O

  15. Search for point-like  sources Equatorial coordinates arXiv:1108.0292v1 [astro-ph.HE] • Two distinct approaches: • all sky search • list of candidates  24 source candidates point-like sources search see J. Gomez’s talk H. Löhner, High Energy Neutrino Flux

  16. Search for diffuse νμ flux • background from • atmospheric : ~ E-3.5 • + prompt neutrinos • cosmic • neutrino models: ~ E-2 • search for high-energy diffuse-flux tail Phys. Lett. B 696 (2011) 16. Energy estimate R based on extra light from delayed OM hits due to high-energy EM showers  no excess of high-energy events above expected flux from atmospheric 

  17. Diffuse flux: upper limits Phys. Lett. B 696 (2011) 16. (334 days of equivalent live time) Upper limit is E2F(E)90%= 4.8×10-8 GeV cm-2 s-1 sr-1 for 20 TeV<E<2.5 PeV

  18. Search for magnetic monopoles Magnetic monopoles emit 8500 more Cherenkov light than a muon  can be detected by ANTARES Selection optimized for the discovery potential (in a blind way) Two estimators to discriminate MM from atmospheric background • The number of hits estimates the quantity of light • The ratio of two tracking reconstruction, λ=log(χ2β=1 /χ2β) where χ2β=1 standard muon algorithm (β =1) χ2β modified algorithm (β free)

  19. Monopoles: upper limits (116 days of equivalent live time with 2008 data)  no excess of events above the expected atmospheric background flux Upper limit is F(E)90%= 1.3×10-17 cm-2 s-1 sr-1 at β≈1

  20. Multimessenger astronomy • Strategy • higher discovery potential by observing different probes • higher significance by coincidence detection • higher efficiency by relaxed cuts SNEWS SuperNova Early Warning System TaToO optical follow up Ligo/Virgo Gravitational waves: trigger + dedicated analysis chain GCN GRB Coord. Network: γ satellites

  21. TAToO project TAToO Optical follow-up of neutrino alerts from ANTARES in order to search for and identify transient sources (GRB, AGN flares…) Reconstruction “on-line” (<10ms) Trigger: multiplet / HE singlet Alert neutrino (GCN) 1.9° x 1.9° ANTARES ν Real time send <10s Tarot and ROTSE Large sky coverage (>2π sr) + high duty cycle Improved sensitivity (1 neutrino may lead to a discovery !!!) No hypothesis on the nature of the source Non dependent on the availability of external triggers Advantages:

  22. Future plans: KM3NeT concept array of multi-PMT optical modules (OM) sensing Cherenkov light instrumented volume several km3 sensitive to all  flavours E > 0.1 GeV angular resolution min 0.1o for E > 10 TeV acceptance: up-going tracks, up to 10o above horizon  

  23. Conclusions ANTARES completed since May 2008 complements the sky coverage of IceCube has a broad physics program new diffuse-flux limit competitive new magnetic monopolesflux limit multi-messenger observations on alert paves the way for KM3NeT