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AGASA Results. Masahiro Teshima Max-Planck-Institut f ü r Physik, M ü nchen, Germany for AGASA collaboration. Cosmic Ray Energy Spectrum. GZK mechanism. N. P. Δ. Super GZK part. ~1/km 2 century. π. γ3K. AGASA Energy Spectrum. AGASA Akeno Giant Air Shower Array. 0 4km.

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Agasa results

AGASA Results

Masahiro Teshima

Max-Planck-Institut für Physik, München, Germany

for AGASA collaboration


Cosmic ray energy spectrum
Cosmic Ray Energy Spectrum

GZK mechanism

P

Δ

Super GZK part.

~1/km2 century

π

γ3K

AGASA Energy Spectrum


Agasa akeno giant air shower array
AGASAAkeno Giant Air Shower Array

0 4km

111 Electron Det.

27 Muon Det.



Detector Calibration in AGASA experiment

Detector Position

Gain as a function of time

(11years data)

Survey from Airplane

ΔX,ΔY=0.1m, ΔZ=0.3m

Cable delay (optic fiber cable)

Accuracy of 100ps by measuring the round trip time in each run

Linearity as a function of time

(11years data)

Detector Gain by muons in each run


Linearity check after dismantling detectors in 2004 Feb

At Akeno Observatory Central building in 2004 Jan


Detector

Response

vertical

θ = 60deg

Detector Housing (Fe 0.4mm)

Detector Box (Fe 1.6mm)

Scintillator (50mm)

Earth (Backscattering)

Detector Simulation (GEANT)

Energy spectra of shower particles


Energy determination
EnergyDetermination

  • Local density at 600m

    • Good energy estimator by M.Hillas

E=2.13x1020eV


The highest energy event
The Highest Energy Event

2.5 x1020eV on 10 May 2001


Attenuation curve
Attenuation curve

S(600) vs Nch

1018eV Proton

Atmospheric depth


S600 attenuation curve
S600 Attenuation curve

20.0

19.5

19.0

18.5

18.0

Atmospheric depth


Proton

S600 Intrinsic fluctuation

Iron


The Conversion

from S600 to Energy

Muon/Neutrino

Ele. Mag


Energy resolution
Energy Resolution

25%

30%

mainly due to measurement errors (particle density measurement and core location determination)not due to shower fluctuation


Major systematics in agasa astro ph 0209422
Major Systematics in AGASAastro-ph/0209422

  • Detector

    • Detector Absolute gain ± 0.7%

    • Detector Linearity ± 7%

    • Detector response(box, housing) ± 5%

  • Energy Estimator S(600)

    • Interaction model, P/Fe, Height ±15%

  • Air shower phenomenology

    • Lateral distribution function ± 7%

    • S(600) attenuation ± 5%

    • Shower front structure ± 5%

    • Delayed particle(neutron) ± 5%

  • Total± 18%


Energy Spectrum by AGASA (θ<45)

11 obs. / 1.8 exp. 4.2σ

5.1 x 1016 m2 s sr


The Energy spectrum by AGASA

Red: well inside the array

(Cut the event near the boundary of array)


Agasa vs hires astro ph
AGASA vs HiRes (astro-ph)

See new paper: Energy determination in AGASA (astro-ph/0209422)


Critical review for energy determination
Critical review for energy determination

  • Fitting the lateral distribution of shower particle density

    • Empirical formula (exclude errors in M.C. but limited by statistics)

      • no energy dependence

      • Linear dependence on sec(theta)

         lateral distribution obtained by Corisika


Lateral distribution
Lateral distribution

Corskika lateral S(600)

Empirical lateral S(600)

Slope parameter eta


S600 attenuation with recent corsika
S600 attenuation with recent Corsika

We are very close to S600 maximum at 1020eV

Overestimation factor

if CORSIKA is right


Preliminary spectra with recent corsika
Preliminary spectra with recent Corsika

Sec(theta) =1.0 - 1.2

Sec(theta) =1.2 - 1.4


Comparison of original energy spectrum and new spectra based on corsika
Comparison of original energy spectrum and new spectra based on Corsika

~10%

~15%

Energy shift

~10% at 1019eV

~15% at 1020eV

to lower direction

Above 1020eV

11events 

5~6 events

Spectrum becomes

more featureless


Auger energy spectrum with fd calibration
Auger Energy Spectrum on Corsikawith FD calibration

AGASA

Corsika

by Arisaka


Auger energy spectrum with mc energy by arisaka
Auger Energy Spectrum on Corsikawith MC energy by Arisaka

AGASA

Corsika

by Arisaka


Arrival direction distribution 4x10 19 ev zenith angle 50deg
Arrival Direction Distribution >4x10 on Corsika19eVzenith angle <50deg.

  • Isotropic in large scale  Extra-Galactic

  • But, Clusters in small scale (Δθ<2.5deg)

    • 1triplet and 6 doublets (2.0 doublets are expected from random)


Space angle distribution of arbitrary two events 4x10 19 ev
Space Angle Distribution of Arbitrary two events >4x10 on Corsika19eV

Normalized sigma

by Li & Ma

3.2 sigma



Space Angle Distribution on Corsika

Log E>19.0

Log E>19.2

Log E>19.4

Log E>19.6


1000 distribution
ρ on Corsikaμ(1000) distribution


Summary
Summary on Corsika

  • Super GZK particles exist

    • Preliminary study with recent CORSIKA

      • If recent CORSIKA describes showers correctly, AGASA energy scale will shift down

        by ~10% at 1019eV and by ~15% at 1020eV on average

      • Spectrum seems to be more featureless (in preliminary study) ??

      • Discrepancy between AGASA and HiRes becomes less significant

  • Small scale anisotropy of UHECR

    • The arrival direction of UHECRs is uniform in large scale

    • But AGASA data shows clusters, 1 triplets and 6 doublets  granularity

    • Source density ~10-5/Mpc3 ~ density of AGNs

    • Re-analysis is on-going with new shower front structure (but very slow)

  • Chemical composition at 1019eV

    • Consistent with light component (P)

    • No gamma ray dominance, γ/all <34%


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