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TUS/KLYPVE SIMULATION

TUS/KLYPVE SIMULATION. D.V. Skobeltsyn Institute of Nuclear Physics, MSU, Moscow, Russia Research and Application Laboratory,MSU, Moscow, Russia Rocket Space Corporation “Energiya”, Korolev, Russia SCTB ‘Luch’, Syzran, Russia Joint Institute for Nuclear Research, Dubna, Russia

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TUS/KLYPVE SIMULATION

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  1. TUS/KLYPVE SIMULATION • D.V. Skobeltsyn Institute of Nuclear Physics, MSU, Moscow, Russia • Research and Application Laboratory,MSU, Moscow, Russia • Rocket Space Corporation “Energiya”, Korolev, Russia • SCTB ‘Luch’, Syzran, Russia • Joint Institute for Nuclear Research, Dubna, Russia • Universidad Autonoma de Puebla, Puebla, Mexico • Instituto de Fisica y Matematicas, U. Michoacan, Mexico • Departemento deFisica, Mexico D. F., Mexico • University of New Mexico, Albuqerque, USA • University of Seoul, Seoul, Korea Dmitry Naumov forCosmotepetl Collaboration

  2. OUTLINE • Introduction • Project objectives • UHECR detection tecniques • TUS: events and background! 2. Simulation • Geometry • Shower development • Fluoresence & Cherenkov • The Earth & Atmosphere 3. Acceptance for TUS & KLYPVE

  3. Project Objectives x = 2.7 x = 3.0 UHECR x = 2.7

  4. Spectrum of UHECR’s

  5. Spectrum of energy Nature (p, Fe, g, n… ) Sources 3 questions = 3 unknowns unknown ! unknown! unknown! • Unknown in addition :Is GZK limit is violated or no ?

  6. UHECR DetectionTecniques Ground based experiments • long history … and now: • AGASA • Hires • P.AUGER • Detect muons • fluorescence • covers 3000 km 2

  7. Space Telescope UHECR ATMOSPHERE TRANSMISSION ’ 20 FLUORESCENCE 10 eV is 6 J! CERENKOV REFLECTION FROM THE EARTH (albédo) UHECR DetectionTecniques Space Telescopes experiments shower energy power 60kW 2

  8. The night view of the EARTH TUS will measure the real background

  9. Existing data SRB Programe : global albedo between 200 and 5000nm TOMS Programe : global albedo between 360 and 380nm Resuls of TOMS: Minimum of the reflection measured by Nimbus 7: ·Continent : 2-4% ·Ocean : 5-8% ·     Cloud : 50% ·Cold cloud/Ice: 90-100% Large seasonal variations Importance of clouds

  10. Clouds Reflection of the Earth 22 june 2002

  11. TUS experimental device The TUS Fresnel mirror operation PMTs Mirror diameter = 1.35 m

  12. TUS mirror production @ JINR

  13. Focal distances agree with expectations within 5cm The light spread on the focal plane is 3-5 mm well below the PMT size

  14. Geometry: 3D Simulations Shower initiated Light Attenuated to the Space Telescope Space Telescope 1. downward showers hitting the FOV surface, 2. downward showers not hitting the FOV surface, 3. upward showers. 2 1 • Earth curvature • Spherical atmosphere 3 • Atmosphere US Standard, Isothermal, LOWTRAN7.1 tabulated profiles.

  15. Shower development Simulations Shower initiated Light Attenuated to the Space Telescope 20 @10 eV • GIL parametrization of CORSIKA for Ne(x) • Hillas parametrization for the energy distribution of electrons • Today the longitudinal profile only is taken into account…the transverse is underway Fe p • SLAST is simulating showers induced by: • Nuclei (p,A) • neutrino

  16. Fluorescence Simulations now Shower initiated Light Attenuated to the Space Telescope • Guner, 1964/Buner, 1967 • Davidson & O’Neil, 1964 • Kakimoto et al 1996 In past • We use Kakimoto et.al fit in (300,400)nm band • Relative intenstities of lines are from Davidson & O’Neil • Other parametrizations are foreseen • Nagano et al, 2000 • ONLY (Palermo,Paris) • Paris low energy spectrometr • AIRFLY (Rome) • FLASH(SLAC) • SLAC • MACFLY(CERN) • Medium energy (Campaninas) • Karlsrhue • Cofin (Italy)

  17. Fluorescence Simulations Shower initiated Light Attenuated to the Space Telescope The fluorescent yield depends on both altitude in the atmosphere and the shower age 337 337 nm 357 nm 391 nm

  18. Cherenkov light simulation Simulations Shower initiated Light Attenuated to the Space Telescope Takes into account • refractive index as a function of the atmosphere state (T,P,water content, etc) • energy distribution of electrons in shower • Light travel time Both fluoresent and cherenkov signals are delayed to due refractive index… few nsec

  19. Atmosphere response Simulations Shower initiated Light Attenuated to the Space Telescope An example from LOWTRAN7.1: a vertical transmission from h to infty h=100 km Two options: • Analytic treatment: Rayleigh & Mie scattering • LOWTRAN7.1 (default) an interface to lowtran is written  LOWTRAN is a part of SLAST h=0 km

  20. Multiple scattering effects (preliminary) Simulations Shower initiated Light Attenuated to the Space Telescope E.Plagnol (Paris) Rayleigh scattering effect on the cherenkov light

  21. Simulations Triggermulti-level triggering 1) Amplitude 2) Duration 3) Pixel correlations TS input TS output Signal Background

  22. Expected events per year(in 1019 eV interval) Simulations Based on AGASA data TUS/KLYPVE in the world AUGER Possible calibration with AUGER EUSO KLYPVE proton TUS Energy, eV

  23. Expected events per year(in 1019 eV and 100 interval) Simulations Based on AGASA data proton TUS KLYPVE Events/year incoming detected Incident angle, deg. Incident angle, deg.

  24. Expected events per year(in 1019 eV and 100 interval) Simulations Based on AGASA data neutrino TUS KLYPVE Events/year incoming detected Incident angle, deg. Incident angle, deg.

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