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Euso Project
Euso Physics
Detection of UHECR showers through fluorescence + Cerenkov
Euso detector : who is doing what ?
Acceptance et counting rates
q andE Horizontal showers and neutrinos
LPM effect
Euso status : NASA, ESA,
B phase and after
Conclusions
and the Lidar
P. Gorodetzky, J. Dolbeau, T. Patzak, E. Plagnol, P. Salin
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EUSO Physics I
Euso objective : Physics above the GZK effect
Extreme energies 1020-1021 eV physicsAstronomy through UHECR and neutrinos
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Euso Physics II
A non observation of the GZK effect would open the road to "new physics" :
Topological defects, Super-massive particules,
Lorentz invariance.
But does not close the door to a classical explanation :
Strong magnetic fields ( 0.1G et Fe) influence, (Astro-Ph/0209192v1) :
Magnetic fields generate isolation zones
(< 10 Mpc):
no exits, no returns
Isotropy
Caustics effects on the doublets.
High statistics are necessary
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Euso Physics III
The AUGER detector will solve the Agasa-Hires case
However, its rate (60evts/year for E>1020eV (if E-2.7)) will limit its ability
to study the UHECR above 1020eV.
WhateverAUGER solution is :
EUSO will be able to study, in a detailed manner, physics above the GZK
cutoff,
EUSO will be able to study the new physics (Super-GZK) or the ones of the
strong magnetic fields (isotropy, correlation).
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UHECR shower detection by fluorescence
Original idea by John Linsley in 1979 (Airwatch)
Large observation area, jumbo mass and, above 5 kmimmune from aerosols
A UHECR shower is seen as the displacement of a particules front.A fraction (
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The EUSO detector : Who does what ?
Optics : USAf 2m
Photo-detector : Japan
200000 pixels
Mechanics : France - Italy
Electronics : France - Italy
Analog - Digital
Ground Segment : Portugal
S.A. (LIDAR) : Switzerland- Italy
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US Optics I
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US Optics II
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French activities : LAPP, LPSC et APC/PCC Annecy Grenoble Collge de France
Analog electronics
Front End
Mechanics and thermal
study of the focal surface
Simulations - ESAF
Atmosphere
Analysis, LidarCommunication
OutreachF.Vannucci
Thermal conductivity of FSA(Summer, 6 m2, 850/200W)
Text-Tint
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Japan
Italy-Alenia
USA
And elsewhere
ESA
USA
Germany
(Munich)
calibrations
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Acceptance and counting rates I
Shower, detector and trigger simulation:
Shower production : Corsika -> parameterization GIL
Photons production : Fluorescence (Kakimoto et al.) and Cerenkov
Atmospheretransport : Rayleigh, Mie, Ozone (LOWTRAN7)
Optics : Transfers and aberrations
Photo-detectors : Filters and quantum efficiency
Trigger : Thresholds and persistence (Nthre, Npers)
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Acceptance and counting rates II
The absolute threshold is anchored by W and the detection efficiency.
The trigger performances determine the acceptance evolution versus energy.
The asymptotic efficiency will be
determined by the cloud coverage.
Efficiency times the power -2.7 law
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Clouds effects I
The cloud coverage will play an important role :
Eventually mask part of the shower (Smax
),
Increase the Cerenkov light reflection;
The cloud coverage is given by the ISCCP database : 280x280 km2 pixel size:
Longitude, latitude, every 3 hours --> altitude, albedo, cloud fraction.
AA Workshop
(GDR-PCHE)-----
LMD (X)
Weather forecast.
Aeronomy (Jussieu)
-----
CelesteHess
Magic
Auger
Euso
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Clouds effects II
Clouds reduce efficiency from 86% 53%
NO CLOUDS CLOUDS
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Clouds effects versus shower energy
E = 5 1019eV E = 5 1020eVE = 1020eV
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Duty cycle
Duty cycle (time fraction usable for measurements) depends on the "photon
background" :Without moon, this background is estimated (measured) to 300 ph/m2/nsec/sr
It originates from the stars light and to the "Airglow"
It does not depend critically on the cloud coverage ( +20%)
Moonlight will limit the duty cycle.
for12.8% of the time, moon is under horizon, for 18% light increase is insignificant,
for 25% light increase < 100 ph/m2/nsec/sr.
To that, too short nights have to be
removed (
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Counting rates
Super-GZK Hypothesis... Or GZK
12% --> 1000 events @ E>1020eV for 25 %
EUSO asymptotic acceptance (>1020eV) represents 5 and 10 times AUGERs
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A possible measurement (duty cycle 12%)
NevtGZK (E>1020eV) >100
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Angular resolution
Precise showers analysis will be made on an event by event basis: each shower
will get errors specifically depending of the observation conditions.As of today, only a statistical error estimation is considered.
Angularresolution : q < 1 ifqshower>60
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Horizontal showers and Neutrinos
Shower length depends on the encountered mass
Fluorescence production (O2
being a quencher) depends only on distance
(altitude < 15km)
Shower width (T) will then depend only on altitude.
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Neutrinos and Hadrons showers
The probability to observe an ( horizontal) hadronic shower with a maximum
under 10km is extremely weak.
Instead, this probability is maximum for neutrinos.
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Euso status : NASA, ESA,
International
NASA has given its OK to EUSO (if ESA ok) : 28 M$
Switzerland will take part to the Lidar study
Germany is officially part of EUSO : H.Teshima (Max Planck, Munich)
ESA
EUSO depends on 2 ESA managements: Science et Manned flights
ESA phase A has ended in July (instrument) and September (Lidar)
ESA committees will decree at the end the year on the project and its transition in
phase B
Management et Collaboration
Euso management structure will evolve : agencies consortium In France a collaboration with AUGER is taking form : AAA, fluorescence, flux
comparison, hybrid events Contacts also with AGASA and HIRES.
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Conclusions
EUSO physics are at the borders of new physics and of our universe understanding, via its
most energetic manifestations.
EUSO detector will be able, after AUGER, to study physics beyond 1020eV with importantstatistics (fluxes, correlations, GZK recovery,) whatever will be the AUGER results on the
Agasa-HiRes case.
Neutrino physics are within range.
Detection (optics, MAPMT) enhancement should allow a decrease of the detection threshold : 2-3 1019eV.
EUSO detector represents the first generation of spatial detectors using the atmosphere as
medium : USA and Japan are already studying the next generation.
The observable mass by EUSO is 2.0 1012 tons with a good transparency
it is an opening on future
At the international level, USA are waiting for the ESA decision.
All laboratories have played a strong role during PhaseA. They are ready to start phase B et
and be even more important there :
Electronics, mechanics, lidar, simulations and analysis...
We are all ready to take a very important place in this project.
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The atmospheric probe : a Lidar ?
Atmosphere is a complex medium and its exploitation (as a detector seen from space) is only
beginning.
Clouds (and other aerosols) treatment needs a control of the atmosphere conditions.A LIDAR(Light Imaging And Ranging) is the most efficient instrument for that : It allows an
(almost) direct measurementof the transmission coefficients.
It is however a complex tool, requiring an important electrical power.
For EUSO it is an important choice which is discussed !
Example of a Laser (355nm)
with EUSO as receiver
No clouds Subvisible clouds
A LIDAR will also allow a
statistical analysis of the clouds
presence
Altitude (km)Altitude (km)
(From G.Fiocco (Rome))