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Topics. Why … Detector Scale Event rate: flux, cross-section Area/Volume etc. Threshold Detector Strategy Optical Radio concept Coherent Radiation from Showers Radio Acoustic. Extreme Sources. NRAO/AUI. UHE Propagation & GZK process. CMBR is opaque. ??. Galactic SN shock.

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  1. D. Seckel, Univ. of Delaware

  2. Topics • Why … • Detector Scale • Event rate: flux, cross-section • Area/Volume etc. • Threshold • Detector Strategy • Optical • Radio concept • Coherent Radiation from Showers • Radio • Acoustic

  3. Extreme Sources NRAO/AUI

  4. UHE Propagation & GZK process CMBR is opaque ?? Galactic SN shock Extra Galactic

  5. “top down” models • Decay/annihilation of defects • Decay of super heavy particles

  6. 1.9 Expectations for n-flux

  7. Event Rates • Rate vs incident flux

  8. Rate v. local flux

  9. Propagation • G is Greens function, determined by solving Boltzman eq. or MC techniques • Includes absorption, downscattering, regeneration, etc • Assume directivity G

  10. Effective Area • For simple propagation

  11. Cross-sections CTEQ-4 • Above PeV, neutrino=anti-neutrino. growth • of parton distribution in nucleon, CC ~ 2 NC • The Earth becomes opaque at high energy. • Uncertainty ~ 25% CTEQ-4 v. 6 (Aramo et al.)

  12. 1.9 Detector scale: 1 km3 v. 1000 km3 15 18

  13. Detector Strategy • Event types • Visible energy • Signals: optical, radio, acoustic • Attenuation • In-situ/Remote • Medium/Location

  14. Event types

  15. Inelasticity EMC effect

  16. Shower Detection Attenuation Length is critical

  17. In-situ v. Remote

  18. Medium & Location – (of better known efforts – several more)

  19. Optical scenarios • IceCube • Auger • Ocean Observer

  20. IceCube • A bit small – low energy • Low rates • Small acceptance from below • Cosmic Ray Background – muon bundles (veto by IceTop ?) • May have “useful” rate up to ~10 PeV • Measure s ?

  21. IceCube II Upward showers! (Hussain, Mckay, Marfatia, Seckel)

  22. Contained or Uncontained (Yoshida) Events with the same energy ~ 30PeV contained High npe: 107 npe uncontained Low npe: 1000 npe

  23. NPE Distribution Distribution difference between the signals and background! GZK m GZK t Atmospheric m

  24. Zenith Angle Distribution down • Signals peak at horizontal direction • Background distribute over down-going region up GZK m GZK t Atmospheric m

  25. Event Rate with 80 strings GZK m GZK t Atmospheric m GZK m GZK t Atmospheric m IceCube Preliminary GZK m0.35events/year GZK t0.31 events/year Atmospheric m0.033events/year GZK: S. Yoshida et. al. (1997) ApJ 479:547 (m=4, Zmax=4)

  26. AUGER (Let them speak…) • Upward tau’s • Earth skimming • Surface detector • Flourescence detector • Rock density, but area suppressed by projection • Downward events • New showers observed deep in atmosphere • Thin target density

  27. Ocean Observer • Concept only • Cf. OWL, EUSO air shower detection • Pros: • 100 x light yield of flourescence • Compact spot – fast hot pixel • 10 x target mass • Cons: • Interface • Sea conditions • No track

  28. Break • Remainder of detection summary contained in 2nd talk. • Includes discussion of radio technique, and overview of radio experiments.

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