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Detection ot the Highest Energy Cosmic Rays Lecture 1 The Violent Universe

Detection ot the Highest Energy Cosmic Rays Lecture 1 The Violent Universe Nucl Phys B (Proc Suppl) 138 (2005) 465-491 Taup Conference Proceedings 2004 James W. Cronin Les Houches, March 19,2007. Assume E -2.5 spectrum. 4. 5.

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Detection ot the Highest Energy Cosmic Rays Lecture 1 The Violent Universe

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  1. Detection ot the Highest Energy Cosmic Rays Lecture 1 The Violent Universe Nucl Phys B (Proc Suppl) 138 (2005) 465-491 Taup Conference Proceedings 2004 James W. Cronin Les Houches, March 19,2007

  2. Assume E-2.5 spectrum

  3. 4

  4. 5

  5. Two techniques: • detect shower particles on the ground • detect air fluorescence produced by shower particles

  6. Beyond 1500 gm/cm2 electromagnetic particles absorbed. (Highly inclined showers)

  7. 90 % of particles within Moliere radius of ≤ 100 m

  8. Thin scintillators measure principally electrons and positrons. A deep water detector measures roughly the total energy flux of the shower particles at its location.

  9. Note: total energy in entire shower carried by muons ≤ 10%

  10. Energy deposit in 1.2 meters of water

  11. At 1000 meters from core

  12. 9 Signal processing can extract em/muon ratio

  13. Old Shower: pure muons 11

  14. pe /A = (/4)(/rp)Ne pe/A = photoelectrons/meter2 • = photocathode efficiency x mirror reflectivity ~ 0.16 • = fluorescence yield ~ 4.5 UV photons/meter/particle  = 1 degree = 0.0175 rp = perpendicular distance to shower axis ~ 20 km • = attenuation ~ exp(rp/) ~ exp(-20/10) ~ 0.135 Ne = number of charged shower particles ~ 7x109 for 1019 EeV pe/A ~ 50 photoelectrons/meter2/degree

  15. Chii vs time Mono 26.15 ± 0.55 km Hybrid 25.96 ± 0.02 km Calibration with central laser facility and Celeste

  16. 14

  17. 16th

  18. S1000 is Energy parameter 8

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