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

The report discusses the potential capabilities of a non-imaging Cerenkov Array, including its applications for below-the-knee studies. It highlights that Cerenkov light production is significantly more abundant than gamma and electron showers, with flatter lateral distribution similar to muons. A detailed overview of the CASA BLANCA setup is provided, featuring energy ranges, sampling density, and light composition. The proposed design incorporates fluorescence, Cerenkov, and muon arrays while optimizing for energy determination and signature analysis across various compositions.

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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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