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Convergence to GZK prediction in
UHE measurements of the primary
energy spectrum of cosmic rays
J. N. Capdevielle, APC, University Paris [email protected]
OutlineOutline General properties of giant EASGeneral properties of giant EAS The extrapolation at UHEThe extrapolation at UHE The treatment of inclined GAS in AGASAThe treatment of inclined GAS in AGASA The treatment of the vertical energy The treatment of the vertical energy
estimatorestimator Amendments of experimental data and Amendments of experimental data and
general convergence to GZK predictiongeneral convergence to GZK prediction Mass composition at UHEMass composition at UHE
Propagation : coupure GZKGreisen, Zatsepin, Kuzmin
Interaction des hadrons avec le fond de photons à 3K (CMB)
Eseuil = 70 EeV
protons
Les sources doivent être proches !
Individual showersIndividual showers
Differential Primary Energy Spectrum of Cosmic Rays
Isotropic distribution of sources
1 = 500 g/cm2 2 = 594 g/cm2
AGASA conversion 600 600
Treatment of inclined EAS data from surface arrays and GZK prediction
Jean Noël CAPDEVIELLE, F.COHEN, B.SZABELSKA, J.SZABELSKI
Measured: lateral distribution + direction (θ, φ)
Density (600m, θ) Density(600m, 0) Energy
That conversion is energy/size independent
See J.phys. G 36 (2009) 075203 by J.N.Capdevielle., F. Cohen, B. Szabelska and J. Szabelski for detailed treatment of inclined EAS
Treatment of inclined EAS data from surface arrays and GZK prediction
Jean Noël CAPDEVIELLE, F.COHEN, B.SZABELSKA, J.SZABELSKI
Results of CORSIKAsimulations showcomplicatedand energy dependentform
example:
Conversion to ''vertical density''
Treatment of inclined EAS data from surface arrays and GZK prediction
Jean Noël CAPDEVIELLE, F.COHEN, B.SZABELSKA, J.SZABELSKI
Cascade theory and CORSIKA simulations
results for the highest energies depend on interaction model,but suggest overestimation of energy at AGASA
Treatment of inclined EAS data from surface arrays and GZK prediction
Jean Noël CAPDEVIELLE, F.COHEN, B.SZABELSKA, J.SZABELSKI
From Bergman spectrum to AGASA spectrumusing AGASA conversion
Grey area: D.R.Bergman et al. (HiRes Collaboration) 29th ICRC, Pune, India, 2005
Red points: AGASA energy spectrum
histograms:MC generated spectrum following Bergman approximately recalculated spectrum using AGASA conversion
Treatment of inclined EAS data from surface arrays and GZK prediction
Jean Noël CAPDEVIELLE, F.COHEN, B.SZABELSKA, J.SZABELSKI
How does the conversion to ''vertical density'' work ?
Treatment of inclined EAS data from surface arrays and GZK prediction
• The spectrum from surface array has to be corrected from the overestimation of the primary energy between 10°-35° in the last decade
• the amended spectrum of AGASA (ISVHECRI aug. 06) is progressing in this direction
• The overestimation in AGASA data was coming up to 50% (in reason of the maximum depth given by AUGER) of the special properties of 3D Electromagnetic cascade near maximum
• It could be more for a pure proton component and less in case of a heavy composition
Fluctuations at constant Fluctuations at constant primary energyprimary energy
100 EeV100 EeV
80 EAS80 EAS
Left wing dominated by the effect of cross section
Same EAS taking into account axis localization ( +/-30m)
and density measurement (10% error)
Knee turns from 3 to 5, ankle 3to 2
Statistical knee effect, decreases the population of high energy EAS in the right wing-- Lower <Eo>
Energy Overestimation
Statistical ankle effect , larger population of EAS in right wing- larger <Eo>
Energy Underestimation
Distribution of Energies contributing to S600= 300
Conversion S600 Eo dashed curve both spectra error on axis of 30m, lower curve 50m, 10% on density
Corrections for 11 of the most energetic cascades in AGASA
AGASA (squares), AUGER(discs), HIRES(stars)
EUSO ~ 1000 x AGASA ~ 30 x AugerEUSO (Instantaneous) ~ 5000 x AGASA ~ 150 x Auger
AGASA
JEM-EUSO tilt-mode
JEM-EUSO FoVJEM-EUSO FoV
Principle of EUSOPrinciple of EUSO- first - first remote-sensingremote-sensing from space, opening a new from space, opening a new
window for the highest energy regimewindow for the highest energy regime
From College de France: better data now
TPC-likenaturalchamber
Cf: Ground-based arrays < 100 EUSO(1) Scintillator array,(2)Fluorescence telescope array
1020 eV
ConclusionsConclusions The primary energy measured in giant surface arrays may be
overestimated in two steps.:
1/ conversion of inclined density S600 to vertical density of reference without taking into account the behavahiour of the estimator versus zenith angle when the maximum depth is close of the level of the array
2/ conversion of the vertical density to the primary energy without taking into account the statistical disturbances generated by a knee in the differential primary spectrum
When corrected for both procedures, AGASA data reflects a GZK behaviour of the primary energy spectrum of cosmic rays in agreement with HIRES and AUGER.
PerspectivesPerspectives New chances for Proton &Gamma ray
Astronomy at UHE from ISS with JEM-EUSO
New results of LHC updating the simulation
. Xmax behaviour and change in p-Air
interaction above 3 EeV? Ratio of light at 500g/cm2 to 1100g/cm2
depends on mass (in favour of p composition at UHE for HIRES)
G.COCCONI, 1961
Ne
t
e
r
Cascade électromagnétique Cascade électromagnétique (NKG)(NKG)
Trans GZK AREATrans GZK AREA New scales New scales Adequate Adequate
Advanced Advanced TechnologiesTechnologies
Milesbornes to Milesbornes to Quantum GravityQuantum Gravity
earliest earliest approaches, EUSO approaches, EUSO and JEM-EUSOand JEM-EUSO
Astronomie proton
1000 evts à répartir sur un certain nombre de sources éventuelles avec leur spectre respectif
Fonction Gaussienne hypergéométrique
f(x) = Ne x s-a (1+x) s-b(1+d.x)-c
À angle fixe, il va falloir ajuster les paramètres :a, b, c, r0, r1, , , , r’0 et r’1
Ne , N et “s” sont donnés par la simulation
Avec x = r / r0 et d = r0 / r1Électrons
Muons f(x) = N x - (1+x)-(-)(1+.x)-
Avec x = r / r’0 et = r’
0 / r’1
Treatment of inclined EAS data from surface arrays and GZK prediction
Jean Noël CAPDEVIELLE, F.COHEN, B.SZABELSKA, J.SZABELSKI
Georgi Timofeevich Zatsepin (2006)
Vadim Alekseyevich Kuzmin (2006)
Résultats des Résultats des ajustementsajustements
Résultats des Résultats des ajustementsajustements
Xmax (g/cm2) and Nmax Xmax (g/cm2) and Nmax for p, Fe initiated showersfor p, Fe initiated showers