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Cosmic Ray Measurements with the KASCADE-Grande Experiment

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Cosmic Ray Measurements with the KASCADE-Grande Experiment June 2009 Cosmic Ray Measurements with the KASCADE-Grande Experiment Presentations for the 31st International Cosmic Ray Conference, Łódź, Poland, July 2009 1. Results on the cosmic ray energy spectrum measured with KASCADE-Grande KASCADE-Grande Collaboration, presented by Andreas Haungs 2. Cosmic ray energy spectrum based on shower size measurements of KASCADE-Grande KASCADE-Grande Collaboration, presented by Donghwa Kang 3. The Energy Spectrum of Primary Cosmic Rays Reconstructed with the KASCADE-Grande Muon Data. KASCADE-Grande Collaboration, presented by Juan Carlos Arteaga-Velazquez 4. The all particle energy spectrum of KASCADE-Grande in the energy region 1016 - 1018 eV by means of the Nch - Nμ technique KASCADE-Grande Collaboration, presented by Mario Bertaina 5. Primary energy reconstruction from the S(500) observable recorded with the KASCADE-Grande detector array KASCADE-Grande Collaboration, presented by Gabriel Toma 6. Performance of the KASCADE-Grande array KASCADE-Grande Collaboration, presented by Federico Di Pierro 7. Muonic Component of Air Showers Measured by the KASCADE-Grande Experiment KASCADE-Grande Collaboration, presented by Daniel Fuhrmann 8. The sensitivity of KASCADE-Grande to the cosmic ray primary composition between 1016 and 1018 eV KASCADE-Grande Collaboration, presented by Elena Cantoni 9. A direct measurement of the muon component of air showers by the KASCADE-Grande Experiment KASCADE-Grande Collaboration, presented by Vitor de Souza 10. Study of EAS development with the Muon Tracking Detector in KASCADE-Grande KASCADE-Grande Collaboration, presented by Janusz Zabierowski 11. Lateral distribution of EAS muons measured with the KASCADE-Grande Muon Tracking Detector KASCADE-Grande Collaboration, presented by Pawel Łuczak 12. Muon Production Height and Longitudinal Shower Development in KASCADE-Grande KASCADE-Grande Collaboration, presented by Paul Doll 13. Restoring Azimuthal Symmetry of Lateral Density Distributions of EAS Particles KASCADE-Grande Collaboration, presented by Octavian Sima 14. Quantitative tests of hadronic interaction models with KASCADE-Grande air shower data KASCADE-Grande Collaboration, presented by Jörg R. Hörandel st PROCEEDINGS OF THE 31 ICRC, ŁOD´ Z´ 2009 1 Results on the cosmic ray energy spectrum measured with KASCADE-Grande xi A. Haungs∗, W.D. Apel∗, J.C. Arteagay; , F. Badea∗, K. Bekk∗, M. Bertainaz, J. Blumer¨ ∗;y, H. Bozdog∗ I.M. Brancusx, M. Bruggemann¨ {, P. Buchholz{, E. Cantoniz;k, A. Chiavassaz, xii F. Cossavellay, K. Daumiller∗, V. de Souzay; , F. Di Pierroz, P. Doll∗, R. Engel∗, J. Engler∗, M. Finger∗, D. Fuhrmann∗∗, P.L. Ghiak, H.J. Gils∗, R. Glasstetter∗∗, C. Grupen{, D. Heck∗, xiii J.R. Horandel¨ y; , T. Huege∗, P.G. Isar∗, K.-H. Kampert∗∗, D. Kangy, D. Kickelbick{, H.O. Klages∗, P. Łuczakyy, H.J. Mathes∗, H.J. Mayer∗, J. Milke∗, B. Mitricax, C. Morellok, xiv G. Navarraz, S. Nehls∗, J. Oehlschlager¨ ∗, S. Ostapchenko∗; , S. Over{, M. Petcux, T. Pierog∗, H. Rebel∗, M. Roth∗, H. Schieler∗, F. Schroder¨ ∗, O. Simazz, M. Stumpert¨ y, G. Tomax, G.C. Trincherok, H. Ulrich∗, A. Weindl∗, J. Wochele∗, M. Wommer∗, J. Zabierowskiyy ∗Institut fur¨ Kernphysik, Forschungszentrum Karlsruhe, 76021 Karlsruhe, Germany yInstitut fur¨ Experimentelle Kernphysik, Universitat¨ Karlsruhe, 76021 Karlsruhe, Germany zDipartimento di Fisica Generale dell'Universita,` 10125 Torino, Italy xNational Institute of Physics and Nuclear Engineering, 7690 Bucharest, Romania {Fachbereich Physik, Universitat¨ Siegen, 57068 Siegen, Germany kIstituto di Fisica dello Spazio Interplanetario, INAF, 10133 Torino, Italy ∗∗Fachbereich Physik, Universitat¨ Wuppertal, 42097 Wuppertal, Germany yySoltan Institute for Nuclear Studies, 90950 Lodz, Poland zzDepartment of Physics, University of Bucharest, 76900 Bucharest, Romania xi now at: Universidad Michoacana, Morelia, Mexico xii now at: Universidade de Sa~o Paulo, Instituto de F´ısica de Sa~o Carlos, Brasil xiii now at: Dept. of Astrophysics, Radboud University Nijmegen, The Netherlands xiv now at: University of Trondheim, Norway Abstract. KASCADE-Grande is an extensive air KASCADE-Grande in 2003 by installing a large array 2 shower experiment at Forschungszentrum Karlsruhe, of 37 stations consisting of 10 m scintillation detec- Germany. The present contribution attempts to pro- tors each (fig. 1). KASCADE-Grande [2] provides an 2 vide a synopsis of the actual results of the recon- area of 0.5 km and operates jointly with the exist- struction of the all-particle energy spectrum in the ing KASCADE detectors. The joint measurements with 16 18 range of 10 eV to 10 eV based on four different the KASCADE muon tracking devices are ensured by methods with partly different sources of systematic an additional cluster (Piccolo) close to the center of uncertainties. Since the calibration of the observables KASCADE-Grande for fast trigger purposes. While the in terms of the primary energy depends on Monte- Grande detectors are sensitive to charged particles, the Carlo simulations, we compare the results of the KASCADE array detectors measure the electromagnetic various methods applied to the same sample of component and the muonic component separately. The measured data. muon detectors enable to reconstruct the total number Keywords: High-energy cosmic rays, energy spec- of muons on an event-by-event basis also for Grande trum, KASCADE-Grande triggered events. I. KASCADE-GRANDE II. RECONSTRUCTION Main parts of the experiment are the Grande array Basic shower observables like the core position, angle- spread over an area of 700 × 700 m2, the original KAS- of-incidence, and total number of charged particles are CADE array covering 200×200 m2 with unshielded and provided by the measurements of the Grande stations. A shielded detectors, and additional muon tracking devices. core position resolution of ≈ 5 m, a direction resolution ◦ This multi-detector system allows us to investigate the of ≈ 0:7 , and a resolution of the total particle number in energy spectrum, composition, and anisotropies of cos- the showers of ≈ 15% is reached [3]. The total number mic rays in the energy range up to 1 EeV. The estimation of muons (Nµ resolution ≈ 25%) is calculated using of energy and mass of the primary particles is based on the core position determined by the Grande array and the combined investigation of the charged particle, the the muon densities measured by the KASCADE muon electron, and the muon components measured by the array detectors [4]. Full efficiency for triggering and re- detector arrays of Grande and KASCADE. construction of air-showers is reached at primary energy The multi-detector experiment KASCADE [1] (lo- of ≈ 2 · 1016 eV, slightly varying on the cuts needed cated at 49.1◦n, 8.4◦e, 110 m a.s.l.) was extended to for the reconstruction of the different observables. 2 A. HAUNGS FOR KASCADE-GRANDE - PRIMARY ENERGY SPECTRUM ] ] KASCADE-Array -1 N Proton -15 ch e [m 10 Nch Iron GeV -1 Nm Proton -16 sr 10 Nm Iron dinat -1 s Nch-Nm -2 -17 MTD CD 10 S(50 0) [m y coor 0 10-18 Piccolo Cluster Energy resolution 17 dI/dE sE/E [%] at 10 eV -19 (QGSJet/FLUKA) 10 N -N : 22% (incl. composition) ch µ -20 10 S(500): 22% (incl. composition) Grande stations N : 15%,31% (for primary iron, proton) ch 10-21 Nµ : 19%,28% (for primary iron, proton) trigger-cluster #17 (of 18) 7 7.5 8 8.5 9 primary energy [log(E0/GeV)] Fig. 2: Reconstructed all-particle energy spectrum by x coordinate [m] four different methods applied to KASCADE-Grande data. Given are also the energy resolution for the meth- Fig. 1: Layout of the KASCADE-Grande experiment: ods. The original KASCADE, the distribution of the 37 stations of the Grande array, and the small Piccolo ] 17 -2 Systematic uncertainty in flux at 10 eV (QGSJet/FLUKA) cluster for fast trigger purposes are shown. The outer 12 N -N : 20% (incl. composition) ch µ clusters of the KASCADE array consist of µ- and e/γ- GeV -1 S(500): 37% (incl. composition) detectors, the inner 4 clusters of e/γ-detectors, only. sr N : 12%,20% (for primary iron, proton) ch -1 7 (f p ima y i , p ) s 10 Nµ : 11%,14% or r r ron roton Applying different methods to the same data sample -2 [m 3 has advantages in various aspects: One would expect 0 E ´ the same result for the energy spectrum by all methods 0 when the measurements are accurate enough, when the E 106 reconstructions work without failures, and when the dI/d Nch Proton Monte-Carlo simulations describe correctly the shower Nch Iron N -N development. But, the fact that the various observables Nm Proton ch m S(500) have substantial differences in their composition sen- Nm Iron sitivity hampers a straightforward analysis. However, 7 7.5 8 8.5 9 investigating results of different methods can be used primary energy [Log(E0 /GeV)] 3 to Fig. 3: Same as figure 2, but the flux multiplied by E0 . • cross-check the measurements by different sub- Values for the uncertainty in the flux determination are detectors; given for the different methods. • cross-check the reconstruction procedures; • cross-check the influence of systematic uncertain- ties; and calibrated by Monte-Carlo simulations under αµ • test the sensitivity of the observables to the elemen- the assumption of a dependence E0 / Nµ and a tal composition; particular primary composition [6]. • test the validity of hadronic interaction models • Nch−Nµ-method: This method combines the infor- underlying the simulations. mation provided by the two observables. By help of Monte-Carlo simulations a formula is obtained to III. ANALYSIS calculate the primary energy per individual shower The estimation of the all-particle energy spectrum is on basis of Nch and Nµ. The formula takes into presently based on four different methods using different account the mass sensitivity in order to minimize observables of KASCADE-Grande: the composition dependence. The attenuation is • Nch-method: The reconstructed charge particle corrected for by deriving the formula for different shower size per individual event is corrected for zenith angle intervals independently and combining attenuation by the constant intensity cut method the energy spectrum afterwards [7].
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