Dmitry Naumov - theor.jinr.ru
Transcript of Dmitry Naumov - theor.jinr.ru
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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