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Below the Belt Working Group Report

Below the Belt Working Group Report. C. C. H. Jui April 29, 2005. General Discussion on Apr.27. Working group discussed in general terms the potential capabilities of the proposed non-imaging Cerenkov Array

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Below the Belt Working Group Report

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  1. Below the Belt Working Group Report C. C. H. Jui April 29, 2005

  2. General Discussion on Apr.27 • Working group discussed in general terms the potential capabilities of the proposed non-imaging Cerenkov Array • Some discussions to alternatives (e.g. “Dice”-like imaging Cerenkov detectors, using timing of Cerenkov light…etc…possible applcations to Below-the Knee

  3. Some BLANCA information(Joe Fowler) • There are ~5-6 orders ofm magnitude more Cerenkov photons than gammas and electrons in a shower • The lateral distributions is flatter than electrons: comparable to muons

  4. Basics of the Technique • Light near the core are emitted deeper in the atmosphere

  5. CASA BLANCA and MIA • CASA array: 500m  500m • 144 BLANCA units deployed in pairs • Typical distance between units ~40 m • Energy Range 1014.510 16.5 eV

  6. Typical BLANCAEvent • Shows BLANCA has very dense (overkill) sampling: • Probably light composition: Energy ~5 PeV

  7. Lateral Profile Fitting • Fitted to exponential (inside 120m) + power law (beyond 200m) curve • C120energy • Inner slope s  Xmax • Outer power index b not used

  8. Energy determination and Conversion of inner slope to Xmax

  9. BLANCA Composition Analysis • Composition is fitted in 5 energy bins in the range 1014.510 16.5 eV • Data appeared to require at least p, He, CNO and Fe for reasonable fit.

  10. Proposed Design Schematic • Combination fluorescence + Cerenkov + muon array • 3km  3km • Can probably sparsify the Cerenkov spacing from BLANCA • May need larger light collectors to reach down to 1014 eV

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