Dmitry Naumov. for Cosmotepetl Collaboration

Transcription

1 TUS/KLYPVE SIMULATION Dmitry Naumov for Cosmotepetl Collaboration 1. D.V. Skobeltsyn Institute of Nuclear Physics, MSU, Moscow, Russia 2. Research and Application Laboratory,MSU, Moscow, Russia 3. Rocket Space Corporation Energiya, Korolev, Russia 4. SCTB Luch, Syzran, Russia 5. Joint Institute for Nuclear Research, Dubna, Russia 6. Universidad Autonoma de Puebla, Puebla, Mexico 7. Instituto de Fisica y Matematicas, U. Michoacan, Mexico 8. Departemento de Fisica, Mexico D. F., Mexico 9. University of New Mexico, Albuqerque, USA 10. University of Seoul, Seoul, Korea 1

2 OUTLINE 1. 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 2

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

4 Spectrum of UHECR s Φ(E) E3 (ev 2m-2 s -1 sr -1 ) AGASA Stereo Fly's Eye Akeno 1 km2 distribution uniforme de sources de z=0.001 à z=1 (spectre source en E -2.5 ) Energie (ev)

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

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

7 UHECR Detection Tecniques Space Telescopes experiments Space Telescope UHECR ATMOSPHERE TRANSMISSION TUS km2 EUSO km2 KLYPVE km2 OWL 2015? shower FLUORESCENCE CERENKOV REFLECTION FROM THE EARTH (albédo) energy ev is 6 J! power 2 60kW 7

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

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

10 Clouds Reflection of the Earth 22 june

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

12 TUS mirror JINR 12

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

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

15 Shower initiated Light Attenuated to the Space Telescope Shower development 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 SLAST is simulating showers induced by: Nuclei (p,a) neutrino ev Fe p 15

16 Shower initiated Light Attenuated to the Space Telescope Fluorescence We use Kakimoto et.al fit in (300,400)nm band Relative intenstities of lines are from Davidson & O Neil Other parametrizations are foreseen 1. Nagano et al, ONLY (Palermo,Paris) 3. Paris low energy spectrometr 4. AIRFLY (Rome) 5. FLASH(SLAC) 6. SLAC 7. MACFLY(CERN) 8. Medium energy (Campaninas) 9. Karlsrhue 10. Cofin (Italy) Guner, 1964/Buner, 1967 Davidson & O Neil, 1964 Kakimoto et al 1996 In past now 16

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

18 Shower initiated Light Attenuated to the Space Telescope Cherenkov light simulation 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 18

19 Shower initiated Light Attenuated to the Space Telescope An example from LOWTRAN7.1: a vertical transmission from h to infty Atmosphere response Two options: 1. Analytic treatment: Rayleigh & Mie scattering h=100 km h=0 km 2. LOWTRAN7.1 (default) an interface to lowtran is written LOWTRAN is a part of SLAST 19

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

21 Trigger multi-level triggering 1) Amplitude 2) Duration 3) Pixel correlations TS input Background Signal TS output 21

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

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

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