1 / 28

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.

justin
Download Presentation

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

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  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

More Related