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TUS/KLYPVE SIMULATIONDmitry 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

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OUTLINE

1. IntroductionProject objectivesUHECR detection tecniquesTUS: events and background!

2. Simulation GeometryShower developmentFluoresence & CherenkovThe Earth & Atmosphere

3. Acceptance for TUS & KLYPVE

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Project Objectives

x = 2.7

x = 3.0

x = 2.7 UHECR

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1023

1024

1025

1026

1017 1018 1019 1020 1021

AGASAStereo Fly's EyeAkeno 1 km2

distribution uniforme de sourcesde z=0.001 à z=1

(spectre source en E-2.5)

Φ(E

) × E

3 (eV

2m

-2s-1

sr-1

)

Energie (eV)

Spectrum of UHECR’s

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3 questions = 3 unknowns

• Spectrum of energy

• Nature (p, Fe, γ, ν… )

• Sources

unknown!

• Unknown in addition :Is GZK limit is violated or no ?

unknown!

unknown !

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UHECR DetectionTecniques

Ground based experiments

long history … and now:

AGASA

Hires

P.AUGER

•Detect muons

•fluorescence

covers 3000 km 2

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UHECR DetectionTecniques

Space Telescopes experiments

2

Space Telescope

UHECR

FLUORESCENCE

CERENKOV

REFLECTION FROM THE EARTH(albédo)

ATMOSPHERETRANSMISSION’

10 eV is 6 J! 20

60kW

shower

energy power

32550 km22009KLYPVE

?2015OWL

150000 km2

2008EUSO

7440 km22005TUS

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The night view of the EARTH

TUS will measure the real background

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Existing data

SRB Programe : global albedo between 200 and 5000 nmTOMS Programe : 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: 90-100%

Large seasonal variationsImportance of clouds

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Clouds

Reflection of the Earth 22 june 2002

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TUS experimental device

The TUS Fresnel mirror operation

PMTs

Mirror diameter = 1.35 m

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TUS mirror production@ JINR

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Focal distances agree with expectations

within 5cm

The light spread on the focal plane is

3-5 mm

well below the PMT size

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Shower initiated Light Attenuated to the Space Telescope

• Geometry: 3D Space Telescope

1. downward showers hitting the FOV surface,2. downward showers not hitting the FOV surface,3. upward showers. 12

3Earth curvatureSpherical atmosphere

•AtmosphereUS Standard, Isothermal, LOWTRAN7.1 tabulated profiles.

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Shower initiated Light Attenuated to the Space Telescope

• Shower development1. GIL parametrization of

CORSIKA for Ne(x)2. Hillas parametrization for the

energy distribution of electrons3. Today the longitudinal profile

only is taken into account…the transverse is underway

@10 eV20

p

Fe

SLAST is simulating showers induced by:• Nuclei (p,A)• neutrino

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Shower initiated Light Attenuated to the Space Telescope

• Fluorescence1. We use Kakimoto et.al fit in

(300,400)nm band2. Relative intenstities of lines are from

Davidson & O’ Neil3. Other parametrizations are foreseen

1. Guner, 1964/Buner, 19672. Davidson & O’Neil, 19643. Kakimoto et al 1996

1. Nagano et al, 20002. ONLY (Palermo,Paris)3. Paris low energy spectrometr4. AIRFLY (Rome)5. FLASH(SLAC)6. SLAC7. MACFLY(CERN)8. Medium energy (Campaninas)9. Karlsrhue10. Cofin (Italy)

In past

now

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Shower initiated Light Attenuated to the Space Telescope

• FluorescenceThe fluorescent yield depends on both altitude in the atmosphere and the shower age

337

337 nm357 nm

391 nm

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Shower initiated Light Attenuated to the Space Telescope

• Cherenkov light simulation

refractive index as a function of the atmosphere state (T,P,water content, etc)

energy distribution of electrons in shower

Takes into account

• Light travel timeBoth fluoresent and cherenkov signals are delayed to due refractive index… few nsec

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Shower initiated Light Attenuated to the Space Telescope

• Atmosphere response

Two options:

1. Analytic treatment: Rayleigh & Mie scattering

2. LOWTRAN7.1 (default)

an interface to lowtran is written

LOWTRAN is a part of SLAST

h=0 km

h=100 km

An example from LOWTRAN7.1: a vertical transmission from h to infty

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Shower initiated Light Attenuated to the Space Telescope

• Multiple scattering

effects (preliminary)

Rayleigh scattering effecton the cherenkov light

E.Plagnol (Paris)

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Triggermulti-level triggering

1) Amplitude 2) Duration 3) Pixel correlations

Signal

Background

TS input TS output

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Expected events per year(in 1019 eV interval)

TUS/KLYPVE in the worldAUGER

KLYPVE

TUS

EUSO

Possible calibration with AUGER

Energy, eV

Based on AGASA data

proton

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Expected events per year(in 1019 eV and 100 interval)

Incident angle, deg. Incident angle, deg.

Events/year

incoming

detected

TUS KLYPVE

Based on AGASA data proton

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Expected events per year(in 1019 eV and 100 interval)

Incident angle, deg. Incident angle, deg.

Events/year

incoming

detected

TUS KLYPVE

Based on AGASA data neutrino