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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

Below the Belt Working Group Report

C. C. H. Jui

April 29, 2005

general discussion on apr 27
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
some blanca information joe fowler
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
basics of the technique
Basics of the Technique
  • Light near the core are emitted deeper in the atmosphere
casa blanca and mia
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
typical blanca event
Typical BLANCAEvent
  • Shows BLANCA has very dense (overkill) sampling:
  • Probably light composition: Energy ~5 PeV
lateral profile fitting
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
blanca composition analysis
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.
proposed design schematic
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