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Comparison of different km3 designs using Antares tools

VLVnT workshop October 2003. Comparison of different km3 designs using Antares tools. D. Zaborov (ITEP, Moscow). Three kinds of detector geometry Incoming muons within 1 .. 1000 TeV energy range Detector efficiency and angular resolution obtained with the Antares tools.

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Comparison of different km3 designs using Antares tools

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  1. VLVnT workshop October 2003 Comparison of different km3 designsusing Antares tools D. Zaborov (ITEP, Moscow) • Three kinds of detector geometry • Incoming muons within 1 .. 1000 TeV energy range • Detector efficiency and angular resolution obtained with the Antares tools

  2. A large homogeneous KM3 detector (8000 PMTs) Structure of the string 20 x 60 m = 1200 m 20 x 60 m = 1200 m 20 x 60 m = 1200 m homogeneous lattice 20 x 20 x 20 downward-looking 10 “ photomultiplier tubes

  3. A large NESTOR – like detector (8750 PMTs) Top view 250 m 250 m 50 floors 20 m step 50 x 20 m = 1000 m 25 towers, each consists of 7 strings PMTs are directed downwards

  4. A large NEMO – like detector (4096 PMTs) 200 m Top view 200 m 20 m 40 m 16 x 40 m = 640 m 16 floors with 4 PMTs each 40 m floor step 64 NEMO - towers

  5. Detector geometries: Common features Set 1: PMTs: 10 inch Characterestics from Antares Hamamatsu R7820 used (eff. Area = 0.44 cm2, angular response, QE) Set 2: 15 inch PMTs: same characteristics but eff. Area = (15/10)2 No PMT multipletts used i.e. Tight coincidences between close PMTs not possible replaced by high pulse condition (above 2.5 , 3.5 pe)

  6. Event Sample Energy range: 1TeV - 1PeV Spectrum: 1/E (flat in log(E)) lower hemisphere isotropic Surface drawing km3 with partic-0.0075 60 (135) kHz noise light Simplified digitisation (2 ARS 25nsec integration) recov4r2 with AartStrategy Analysis antroot and a3d

  7. Program modifications Most of the code was easily scalable for use with 1km3 detector Some parameters in include files had to be changed like: (km3.inc, phomul.inc) max. number of PMTs, clusters, strings Patch work in km3 to allow use of 15 inch PMT without creating new diffusion tables Reco: modification of Select and Filter routines to adapt to high pulse condition and absence of coincidences (2.5 pe for 10 inch PMT, 3.5pe for 15inch PMT)

  8. Modified causality filter Usual filter: abs(dt) < dr/vlight Large detectors (new condition): abs[abs(dt)-dr/clight] < 500nsec Approximation x << dr (hits close to muon track, takes into account absorption) Plane wave approximation dr << x (photon travel path)

  9. Modified causality filter Logical AND between both conditions Old condition Photons travel too far Newly excluded Always Excluded New condition Photon front originates too far away Newly excluded Effective for dr > 150m, probably negligible for 0.1km2 detector

  10. Effect of new causality filter Tails reduced even without quality cuts Eff. Area improved

  11. Angular error distribution with the homogeneous detector integrated over the energy range 1..1000 TeV

  12. Angular resolution of the homogeneous detector

  13. Angular resolution of the NESTOR-like detector

  14. Angular resolution of the NEMO-like detector

  15. Effective area of the homogeneous detector for muons * only statistical errors are shown; K40 noise 60 kHz

  16. Effective area of the NESTOR-like detector for muons

  17. Effective area of the NEMO-like detector for muons

  18. Homogeneous geometry: number of detected hits vs. muon energy Effective “threshold” ~ 15-20 hits

  19. NESTOR-like geometry: number of detected hits vs. muon energy Effective “threshold” now ~ 20-25 hits

  20. NEMO geometry: number of detected hits vs. muon energy Effective “threshold” now ~ 20-25 hits should be reachable ?

  21. Effective area dependence on PMT size At low energies dependence on total photocathode area At high energies dependence on PMT number

  22. Effective area dependence on noise Used reconstruction filters noise hits effectively At low energies lowering thresholds with low noise improves performance

  23. Conclusions • Monte-Carlo simulation of Cherenkov light production and muon track reconstruction have been performed using Antares tools. • The homogeneous geometry demonstrates high detector efficiency starting from 1 TeV. • Effective area reached with the NESTOR-like geometry is smaller than obtained with the homogeneous geometry. • The NEMO-like detector has a significantly smaller effective area than the homogeneous configuration mainly due to its lower PMT density. • All the geometries show angular resolution in muon track reconstruction of about 0.1 degree or better. • High requirements of the reconstruction software for the number of hits, especially with non-homogeneous detectors, have been discovered and require further investigations.

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