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Advancements in Non-Imaging Cerenkov Array for Below-The-Knee Applications

The working group discussed the potential capabilities of the proposed non-imaging Cerenkov Array, focusing on its application in below-the-knee analysis. Compared to traditional gamma and electron detection, Cerenkov emissions exhibit significantly higher photon counts, with flatter lateral distributions resembling those of muons. The CASA BLANCA project was highlighted, featuring a 500m x 500m array with 144 paired units. Initial findings suggest Cerenkov light could enhance energy determination and composition analysis at energies from 10^14.5 to 10^16.5 eV, advocating a combined system with fluorescence and muon detection.

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Advancements in Non-Imaging Cerenkov Array for Below-The-Knee Applications

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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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