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Physics Laboratory

Physics Laboratory. School of Science and Technology. Hellenic Open University. Calibration and Optimization of a Very Large Volume Deep-Sea Neutrino Telescope using Extensive Air Showers. Antonios Leisos. International Workshop On Very large Volume Neutrino Telescopes

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Physics Laboratory

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  1. Physics Laboratory School of Science and Technology Hellenic Open University Calibration and Optimization of a Very Large Volume Deep-Sea Neutrino Telescope using Extensive Air Showers AntoniosLeisos International Workshop On Very large Volume Neutrino Telescopes 13-15 October 2009, Athens, Greece

  2. Outline • Air Shower detection for Deep Sea • ν-Telescope Calibration (updated analysis) • Calibration using single muons or extensive (air) showers? • New Crude Analysis for Optimum angular offset determination (motivated from IceTop Analysis)

  3. A Calibration Study At least one muon with E>2TeV passing through the neutrino telescope dt=0 dt1 μ track dt2 Detailed Simulation (propagation & Energy Loss) dt3 d: distance from the shower axis km3

  4. A Calibration Study 5m 3 stations for 10 days 19m

  5. Comparison of Estimations • Detector: SeaWiet • Depth: 2500 m • Quality cuts: • mean deposited charge in active counters >1.7 • number of PMT hits > 10. φ array Θ array φ telescope Θ telescope σ=47m σ=6.70 σ=420 θTelescope-θarray φTelescope-φarray ΧTelescope-Χarray

  6. Monte carlo Results 3X16 counters 10 days of operation SeaWiet νOne 1000m SeaWiet νOne Can we make it better?

  7. Shower vs Single muon Total number of muons through S for 10 days operation S D *Numbers calculated assuming R0=1km, 30% reconstruction efficiency of ν-Telescope ** Results of MC simulation with full reconstruction (10 % efficiency) R0

  8. DetectorModule GPS timestamp DAQ S/W based on LabView On-Line analysis - distributions Scintillation Tiles WLS fibers

  9. Single p.e Charge (pCb) ModuleCalibration Response to a MIP Detector Uniformity @ “nominal” H.V. gain: ~ 4 105 <charge>/p.e. ~ 0.07pCb <pulse height>/p.e. ~ 1.05mV Typical Mean Numb. of p.e. per m.i.p. : 21 ± 10% variation

  10. Detailed Monte Carlo description Monte Carlo & Data Comparison A1 B2 A3 Input C Trigger B3 A2 B1 At the Detector Center  Data ___ M.C. Prediction • Data - Monte Carlo Prediction μ=-0.1±0.3 σ=7.6 ± 0.2 Charge (in units of mean p.e. charge) θΑ-θΒ

  11. Use IceTop’s Analysis Thomas Geisser (Performance of IceTop Array-ICRC’07 Eμ>2 ΤeV (X0,Y0.Z0) Χμ-Χshower

  12. Crude & Accurate Estimation (XN,YN) Θ 0 d (X0,Y0) θ0-θshower

  13. Angular Offset Resolution ΔΤ~14 hours 16 m2 array 0.050 ΔΤ~1 day 3X16 m2 array 0.020 ΔΤ~10days 3X16 m2 array <0.010 θest-θ0 • Detector: SeaWiet • Depth: 2500 m • Quality cuts: • number of PMT hits > 10.

  14. Low & Higher multiplicity triggers Only 2 counters 2 or more counters • Detector: SeaWiet • Depth: 2500 m • Quality cuts: • number of PMT hits > 10. θest-θ0 θest-θ0

  15. Crude vs Weighted Mean (XN,YN) θest-θ0 Θ w d (Xw,Yw) θest-θw • Detector: SeaWiet • Depth: 2500 m • Quality cuts: • number of PMT hits > 10

  16. Azimuth Offset Resolution φ0-φshower φest-φo • Detector: SeaWiet • Depth: 2500 m • Quality cuts: • number of PMT hits > 10.

  17. Position Correlation Xdet+10m θest-θ0 Xdet+50m Xdet+50m θest-θ0 φest-φo Detector: SeaWiet Depth: 2500 m Quality cuts: number of PMT hits > 10.

  18. Summary Of Results SeaWiet νOne Consistent Estimations when the array Is shifted in X or Y axis

  19. Estimation of the angular resolution of the KM3NeT – (Inter-Calibration) KM3NeT’s resolution measurement Impossible using EAS array KM3NeT resolution ~ 0.1 deg EAS Detector resolution ~ 2 deg (Inter-Calibration) • Divide the detector in 2 identical sub detectors • Reconstruct the muon separately for each sub detector • Compare the 2 reconstructed track directions Working Example IceCube Geometry 9600 OMs looking up & down in a hexagonal grid. 80 Strings, 60 storeys each. 17m between storeys MultiPMT Optical Module 125m

  20. Resolution Estimation (1 TeV Muons, isotropic flux, IceCube Geometry, 9600 OMs) Mean 12 hits Number of active OMs in one subdetector Mean 24 hits Number of active OMs in whole detector • Simulatedevents with at least 14 active OMs, after filtering out the background hits. • The selected sample consisted, in average, of 24active OMs per event, whilst the remaining contamination from K40 backgroundhits was less than 0.5 OM per event. • Each muon track was reconstructed usingthe information from the whole set of the active OMs as well as using the datafrom the two sub-groups, each containing the half of the selected OMs.

  21. Resolution Estimation (1 TeV Muons, isotropic flux, IceCube Geometry, 9600 OMs) Mean 12 hits Number of active OMs in one subdetector Mean 24 hits Number of active OMs in whole detector • Simulatedevents with at least 14 active OMs, after filtering out the background hits. • The selected sample consisted, in average, of 24active OMs per event, whilst the remaining contamination from K40 backgroundhits was less than 0.5 OM per event. • Each muon track was reconstructed usingthe information from the whole set of the active OMs as well as using the datafrom the two sub-groups, each containing the half of the selected OMs.

  22. Resolution Estimation (1 TeV Muons, isotropic flux, IceCube Geometry, 9600 OMs) σ=0.07o±0.003o σ=0.095o ±0.005o Zenith angle resolution of subdetectors (degrees) Zenith angle resolution of whole detector (degrees)

  23. Resolution Estimation (1 TeV Muons, isotropic flux, IceCube Geometry, 9600 OMs) σ=0.14o±0.01o Zenith angle difference between the 2 reconstructed directions (degrees) Space angle difference between the 2 reconstructed directions (degrees) ≈ 0.095o ±0.005o

  24. SeaWiet

  25. νOne

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