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Search Results: 1 - 10 of 455886 matches for " J. C. Arteaga-Velázquez "
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The cosmic ray energy spectrum in the range 1016–1018 eV measured by KASCADE-Grande
M. Bertaina, W.D. Apel, J.C. Arteaga-Velázquez,a, K. Bekk, J. Blümer, H. Bozdog, I.M. Brancus, P. Buchholz, E. Cantoni, A. Chiavassa, F. Cossavella,b, K. Daumiller, V. de Souza,c, F. Di Pierro, P. Doll, R. Engel, J. Engler, M. Finger, D. Fuhrmann, P.L. Ghia, H.J. Gils, R. Glasstetter, C. Grupen, A. Haungs, D. Heck, J.R. H randel,d, T. Huege, P.G. Isar, K.-H. Kampert, D. Kang, D. Kickelbick, H.O. Klages, K. Link, P. uczak, M. Ludwig, H.J. Mathes, H.J. Mayer, M. Melissas, J. Milke, B. Mitrica, C. Morello, G. Navarra,e, S. Nehls, J. Oehlschl ger, S. Ostapchenko,f, S. Over, N. Palmieri, M. Petcu, T. Pierog, H. Rebel, M. Roth, H. Schieler, F. Schr der, O. Sima, G. Toma, G.C. Trinchero, H. Ulrich, A. Weindl, J. Wochele, M. Wommer,J. Zabierowski
Astrophysics and Space Sciences Transactions (ASTRA) , 2011, DOI: 10.5194/astra-7-229-2011
Abstract: The KASCADE-Grande experiment, located at Campus North of the Karlsruhe Institute of Technology (Germany) is a multi-component extensive air-shower experiment devoted to the study of cosmic rays and their interactions at primary energies 1014–1018 eV. One of the main goals of the experiment is the measurement of the all particle energy spectrum in the 1016–1018 eV range, i.e. extending the range accessible by KASCADE alone. The Grande detector samples the charged component (Nch) of the air shower while the original KASCADE array provides in addition a measurement of the muon component (Nμ). The combined information of Nch and Nμ is used to estimate the energy on an event-by-event basis and to derive the all-particle energy spectrum. Since the calibration of the observables in terms of the primary energy depends on Monte Carlo simulations, three different methods with partially different sources of uncertainties, have been considered and compared to each other to derive the systematics on the energy spectrum. The different methods employed to derive the spectrum and their uncertainties, as well as the implications of the obtained result, are discussed in detail.
The study in the primary energy range 10^{16} - 10^{17} eV with the Muon Tracking Detector in the KASCADE-Grande experiment
P. ?uczak,W. D. Apel,J. C. Arteaga-Velázquez,K. Bekk,M. Bertaina,J. Blümer,H. Bozdog,I. M. Brancus,E. Cantoni,A. Chiavassa,F. Cossavella,C. Curcio,K. Daumiller,V. de Souza,F. Di Pierro,P. Doll,R. Engel,J. Engler,B. Fuchs,D. Fuhrmann,H. J. Gils,R. Glasstetter,C. Grupen,A. Haungs,D. Heck,J. R. H?randel,D. Huber,T. Huege,K. -H. Kampert,D. Kang,H. O. Klages,K. Link,M. Ludwig,H. J. Mathes,H. J. Mayer,M. Melissas,J. Milke,B. Mitrica,C. Morello,J. Oehlschl?ger,S. Ostapchenko,N. Palmieri,M. Petcu,T. Pierog,H. Rebel,M. Roth,H. Schieler,S. Schoo,F. G. Schr?der,O. Sima,G. Toma,G. C. Trinchero,H. Ulrich,A. Weindl,J. Wochele,J. Zabierowski
Physics , 2013,
Abstract: The KASCADE-Grande Muon Tracking Detector enables with high accuracy the measurement of directions of EAS muons with energy above 0.8 GeV and up to 700 m distance from the shower centre. Reconstructed muon tracks are used to investigate muon pseudorapidity (eta) distributions. These distributions are nearly identical to the pseudorapidity distributions of their parent mesons produced in hadronic interactions. Comparison of the eta distributions from measured and simulated showers can be used to test the quality of the high energy hadronic interaction models. In this context a comparison of the QGSJet-II-2 and QGSJet-II-4 model will be shown. The pseudorapidity distributions reflect the longitudinal development of EAS and, as such, are sensitive to the mass of the cosmic rays primary particles. With various parameters of the eta distribution, obtained from the MTD data, it is possible to calculate the mean logarithmic mass of CRs. The results of the analysis in the primary energy range 10^{16} eV - 10^{17} eV with the 1st quartile (Q1) of eta distribution will be presented.
Comparison of LOPES data and CoREAS simulations using a full detector simulation (ICRC2013)
K. Link,W. D. Apel,J. C. Arteaga-Velázquez,L. B?hren,K. Bekk,M. Bertaina,P. L. Biermann,J. Blümer,H. Bozdog,I. M. Brancus,E. Cantoni,A. Chiavassa,K. Daumiller,V. De Souza,F. Di Pierro,P. Doll,R. Engel,H. Falcke,B. Fuchs,D. Fuhrmann,H. Gemmeke,C. Grupen,A. Haungs,D. Heck,J. R. H?randel,A. Horneffer,D. Huber,T. Huege,P. G. Isar,K-H. Kampert,D. Kang,O. Kr?mer,J. Kuijpers,P. ?Uczak,M. Ludwig,H. J. Mathes,M. Melissas,C. Morello,J. Oehlschl?ger,N. Palmieri,T. Pierog,J. Rautenberg,H. Rebel,M. Roth,C. Rühle,A. Saftoiu,H. Schieler,A. Schmidt,F. G. Schr?der,O. Sima,G. Toma,G. C. Trinchero,A. Weindl,J. Wochele,J. Zabierowski,J. A. Zensus
Physics , 2013,
Abstract: The LOPES experiment at the Karlsruhe Institute of Technology, Germany, has been measuring radio emission of air showers for almost 10 years. For a better understanding of the emission process a detailed comparison of data with simulations is necessary. This is possible using a newly developed detector simulation including all LOPES detector components. After propagating a simulated event through this full detector simulation a standard LOPES like event file is written. LOPES data and CoREAS simulations can then be treated equally and the same analysis software can be applied to both. This gives the opportunity to compare data and simulations directly. Furthermore, the standard analysis software can be used with simulations which provide the possibility to check the accuracy regarding reconstruction of air shower parameters. We point out the advantages and present first results using such a full LOPES detector simulation. A comparison of LOPES data and the Monte Carlo code CoREAS based on an analysis using this detector simulation is shown.
The wavefront of the radio signal emitted by cosmic ray air showers
W. D. Apel,J. C. Arteaga-Velázquez,L. B?hren,K. Bekk,M. Bertaina,P. L. Biermann,J. Blümer,H. Bozdog,I. M. Brancus,E. Cantoni,A. Chiavassa,K. Daumiller,V. de Souza,F. Di Pierro,P. Doll,R. Engel,H. Falcke,B. Fuchs,H. Gemmeke,C. Grupen,A. Haungs,D. Heck,J. R. H?randel,A. Horneffer,D. Huber,T. Huege,P. G. Isar,K. -H. Kampert,D. Kang,O. Kr?mer,J. Kuijpers,K. Link,P. Luczak,M. Ludwig,H. J. Mathes,M. Melissas,C. Morello,J. Oehlschl?ger,N. Palmieri,T. Pierog,J. Rautenberg,H. Rebel,M. Roth,C. Rühle,A. Saftoiu,H. Schieler,A. Schmidt,S. Schoo,F. G. Schr?der,O. Sima,G. Toma,G. C. Trinchero,A. Weindl,J. Wochele,J. Zabierowski,J. A. Zensus
Physics , 2014, DOI: 10.1088/1475-7516/2014/09/025
Abstract: Analyzing measurements of the LOPES antenna array together with corresponding CoREAS simulations for more than 300 measured events with energy above $10^{17}\,$eV and zenith angles smaller than $45^\circ$, we find that the radio wavefront of cosmic-ray air showers is of approximately hyperbolic shape. The simulations predict a slightly steeper wavefront towards East than towards West, but this asymmetry is negligible against the measurement uncertainties of LOPES. At axis distances $\gtrsim 50\,$m, the wavefront can be approximated by a simple cone. According to the simulations, the cone angle is clearly correlated with the shower maximum. Thus, we confirm earlier predictions that arrival time measurements can be used to study the longitudinal shower development, but now using a realistic wavefront. Moreover, we show that the hyperbolic wavefront is compatible with our measurement, and we present several experimental indications that the cone angle is indeed sensitive to the shower development. Consequently, the wavefront can be used to statistically study the primary composition of ultra-high energy cosmic rays. At LOPES, the experimentally achieved precision for the shower maximum is limited by measurement uncertainties to approximately $140\,$g/cm$^2$. But the simulations indicate that under better conditions this method might yield an accuracy for the atmospheric depth of the shower maximum, $X_\mathrm{max}$, better than $30\,$g/cm$^2$. This would be competitive with the established air-fluorescence and air-Cherenkov techniques, where the radio technique offers the advantage of a significantly higher duty-cycle. Finally, the hyperbolic wavefront can be used to reconstruct the shower geometry more accurately, which potentially allows a better reconstruction of all other shower parameters, too.
Revised absolute amplitude calibration of the LOPES experiment
K. Link,T. Huege,W. D. Apel,J. C. Arteaga-Velázquez,L. B?hren,K. Bekk,M. Bertaina,P. L. Biermann,J. Blümer,H. Bozdog,I. M. Brancus,E. Cantoni,A. Chiavassa,K. Daumiller,V. de Souza,F. Di Pierro,P. Doll,R. Engel,H. Falcke,B. Fuchs,H. Gemmeke,C. Grupen,A. Haungs,D. Heck,R. Hiller,J. R. H?randel,A. Horneffer,D. Huber,P. G. Isar,K-H. Kampert,D. Kang,O. Kr?mer,J. Kuijpers,P. ?uczak,M. Ludwig,H. J. Mathes,M. Melissas,C. Morello,J. Oehlschl?ger,N. Palmieri,T. Pierog,J. Rautenberg,H. Rebel,M. Roth,C. Rühle,A. Saftoiu,H. Schieler,A. Schmidt,S. Schoo,F. G. Schr?der,O. Sima,G. Toma,G. C. Trinchero,A. Weindl,J. Wochele,J. Zabierowski,J. A. Zensus
Physics , 2015,
Abstract: One of the main aims of the LOPES experiment was the evaluation of the absolute amplitude of the radio signal of air showers. This is of special interest since the radio technique offers the possibility for an independent and highly precise determination of the energy scale of cosmic rays on the basis of signal predictions from Monte Carlo simulations. For the calibration of the amplitude measured by LOPES we used an external source. Previous comparisons of LOPES measurements and simulations of the radio signal amplitude predicted by CoREAS revealed a discrepancy of the order of a factor of two. A re-measurement of the reference calibration source, now performed for the free field, was recently performed by the manufacturer. The updated calibration values lead to a lowering of the reconstructed electric field measured by LOPES by a factor of $2.6 \pm 0.2$ and therefore to a significantly better agreement with CoREAS simulations. We discuss the updated calibration and its impact on the LOPES analysis results.
The KASCADE-Grande experiment: measurements of the all-particle energy spectrum of cosmic rays
J. C. Arteaga-Velázquez,W. D. Apel,K. Bekk,M. Bertaina,J. Blümer,H. Bozdog,I. M. Brancus,P. Buchholz,E. Cantoni,A. Chiavassa,F. Cossavella,K. Daumiller,V. de Souza,F. Di Pierro,P. Doll,R. Engel,J. Engler,M. Finger,D. Fuhrmann,P. L. Ghia,H. J. Gils,R. Glasstetter,C. Grupen,A. Haungs,D. Heck,J. R. H?randel,T. Huege,P. G. Isar,K. -H. Kampert,D. Kickelbick,H. O. Klages,K. Link,P. Luczak,M. Ludwig,H. J. Mathes,H. J. Mayer,M. Melissas,J. Milke,B. Mitrica,C. Morello,G. Navarra,S. Nehls,J. Oehlschl?ger,S. Ostapchenko,S. Over,N. Palmieri,M. Petcu,T. Pierog,H. Rebel,M. Roth,H. Schieler,F. Schr?der,O. Sima,G. Toma,G. C. Trinchero,H. Ulrich,A. Weindl,J. Wochele,M. Wommer,J. Zabierowski
Physics , 2010,
Abstract: The all-particle energy spectrum as measured by the KASCADE-Grande experiment for E = 10^{16} - 10^{18} eV is presented within the framework of the QGSJET II/FLUKA hadronic interaction models. Three different methods were applied based on the muon size and the total number of charged particles individually and in combination. From the study it is found that the spectrum cannot be completely described by a smooth power law due to the presence of characteristic features.
Sensitivity of KASCADE-Grande data to hadronic interaction models
D. Kang,W. D. Apel,J. C. Arteaga-Velázquez,K. Bekk,M. Bertaina,J. Blümer,H. Bozdog,I. M. Brancus,P. Buchholz,E. Cantoni,A. Chiavassa,F. Cossavella,K. Daumiller,V. de Souza,F. di Pierro,P. Doll,R. Engel,J. Engler,M. Finger,D. Fuhrmann,P. L. Ghia,H. J. Gils,R. Glasstetter,C. Grupen,A. Haungs,D. Heck,J. R. H?randel,T. Huege,P. G. Isar,K. -H. Kampert,D. Kickelbick,H. O. Klages,K. Link,P. Luczak,M. Ludwig,H. J. Mathes,H. J. Mayer,M. Melissas,J. Milke,B. Mitrica,C. Morello,G. Navarra,S. Nehls,J. Oehlschl?ger,S. Ostapchenko,S. Over,N. Palmieria,M. Petcu,T. Pierog,H. Rebel,M. Roth,H. Schieler,F. G. Schr?der,O. Sima,G. Toma,G. C. Trinchero,H. Ulrich,A. Weindl,J. Wochele,M. Wommer,J. Zabierowski
Physics , 2010,
Abstract: KASCADE-Grande is a large detector array dedicated for studies of high-energy cosmic rays in the primary energy range from 100 TeV to 1 EeV. The multi-detector concept of the experimental set-up offers the possibility to measure simultaneously various observables related to the electromagnetic, muonic, and hadronic air shower components. The experimental data are compared to predictions of CORSIKA simulations using high-energy hadronic interaction models (e.g. QGSJET or EPOS), as well as low-energy interaction models (e.g. FLUKA or GHEISHA). This contribution will summarize the results of such investigations. In particular, the validity of the new EPOS version 1.99 for EAS with energy around 100 PeV will be discussed.
KASCADE-Grande measurements of energy spectra for elemental groups of cosmic rays
The KASCADE-Grande Collaboration,:,W. D. Apel,J. C. Arteaga-Velàzquez,K. Bekk,M. Bertaina,J. Blümer,H. Bozdog,I. M. Brancus,E. Cantoni,A. Chiavassa,F. Cossavella,K. Daumiller,V. de Souza,F. Di Pierro,P. Doll,R. Engel,J. Engler,M. Finger,B. Fuchs,D. Fuhrmann,H. J. Gils,R. Glasstetter,C. Grupen,A. Haungs,D. Heck,J. R. H?randel,D. Huber,T. Huege,K. -H. Kampert,D. Kang,H. O. Klages,K. Link,P. ?uczak,M. Ludwig,H. J. Mathes,H. J. Mayer,M. Melissas,J. Milke,B. Mitrica,C. Morello,J. Oehlschl?ger,S. Ostapchenko,N. Palmieri,M. Petcu,T. Pierog,H. Rebel,M. Roth,H. Schieler,S. Schoo,F. G. Schr?der,O. Sima,G. Toma,G. C. Trinchero,H. Ulrich,A. Weindl,J. Wochele,M. Wommer,J. Zabierowski
Physics , 2013, DOI: 10.1016/j.astropartphys.2013.06.004
Abstract: The KASCADE-Grande air shower experiment [W. Apel, et al. (KASCADE-Grande collaboration), Nucl. Instrum. Methods A 620 (2010) 202] consists of, among others, a large scintillator array for measurements of charged particles, Nch, and of an array of shielded scintillation counters used for muon counting, Nmu. KASCADE-Grande is optimized for cosmic ray measurements in the energy range 10 PeV to about 2000 PeV, where exploring the composition is of fundamental importance for understanding the transition from galactic to extragalactic origin of cosmic rays. Following earlier studies of the all-particle and the elemental spectra reconstructed in the knee energy range from KASCADE data [T. Antoni, et al. (KASCADE collaboration), Astropart. Phys. 24 (2005) 1], we have now extended these measurements to beyond 200 PeV. By analysing the two-dimensional shower size spectrum Nch vs. Nmu for nearly vertical events, we reconstruct the energy spectra of different mass groups by means of unfolding methods over an energy range where the detector is fully efficient. The procedure and its results, which are derived based on the hadronic interaction model QGSJET-II-02 and which yield a strong indication for a dominance of heavy mass groups in the covered energy range and for a knee-like structure in the iron spectrum at around 80 PeV, are presented. This confirms and further refines the results obtained by other analyses of KASCADE-Grande data, which already gave evidence for a knee-like structure in the heavy component of cosmic rays at about 80 PeV [W. Apel, et al. (KASCADE-Grande collaboration), Phys. Rev. Lett. 107 (2011) 171104].
Longitudinal EAS-Development Studies in the Air-Shower Experiment KASCADE-Grande
P. Doll,W. D. Apel,J. C. Arteaga-Velázquez,K. Bekk,M. Bertaina,J. Blümer,H. Bozdog,I. M. Brancus,P. Buchholz,E. Cantoni,A. Chiavassa,F. Cossavella,K. Daumiller,V. de Souza,F. di Pierro,R. Engel,J. Engler,M. Finger,D. Fuhrmann,P. L. Ghia,H. J. Gils,R. Glasstetter,C. Grupen,A. Haungs,D. Heck,J. R. H?randel,T. Huege,P. G. Isar,K. -H. Kampert,D. Kang,D. Kickelbick,H. O. Klages,K. Link,P. ?uczak,M. Ludwig,H. J. Mathes,H. J. Mayer,M. Melissas,J. Milke,B. Mitrica,C. Morello,G. Navarra,S. Nehls,J. Oehlschl?ger,S. Ostapchenko,S. Over,N. Palmieria,M. Petcu,T. Pierog,H. Rebel,M. Roth,H. Schieler,F. G. Schr?der,O. Sima,G. Toma,G. C. Trinchero,H. Ulrich,A. Weindl,J. Wochele,M. Wommer,J. Zabierowski
Physics , 2010,
Abstract: A large area (128 m^2) Muon Tracking Detector (MTD), located within the KASCADE experiment, has been built with the aim to identify muons (E_mu > 0.8 GeV) and their directions in extensive air showers by track measurements under more than 18 r.l. shielding. The orientation of the muon track with respect to the shower axis is expressed in terms of the radial- and tangential angles. By means of triangulation the muon production height H_mu is determined. By means of H_mu, a transition from light to heavy cosmic ray primary particle with increasing shower energy Eo from 1-10 PeV is observed. Muon pseudorapidity distributions for the first interactions above 15 km are studied and compared to Monte Carlo simulations.
Ankle-like Feature in the Energy Spectrum of Light Elements of Cosmic Rays Observed with KASCADE-Grande
W. D. Apel,J. C. Arteaga-Velàzquez,K. Bekk,M. Bertaina,J. Blümer,H. Bozdog,I. M. Brancus,E. Cantoni,A. Chiavassa,F. Cossavella,K. Daumiller,V. de Souza,F. Di Pierro,P. Doll,R. Engel,J. Engler,M. Finger,B. Fuchs,D. Fuhrmann,H. J. Gils,R. Glasstetter,C. Grupen,A. Haungs,D. Heck,J. R. H?randel,D. Huber,T. Huege,K. -H. Kampert,D. Kang,H. O. Klages,K. Link,P. ?uczak,M. Ludwig,H. J. Mathes,H. J. Mayer,M. Melissas,J. Milke,B. Mitrica,C. Morello,J. Oehlschl?ger,S. Ostapchenko,N. Palmieri,M. Petcu,T. Pierog,H. Rebel,M. Roth,H. Schieler,S. Schoo,F. G. Schr?der,O. Sima,G. Toma,G. C. Trinchero,H. Ulrich,A. Weindl,J. Wochele,M. Wommer,J. Zabierowski
Physics , 2013, DOI: 10.1103/PhysRevD.87.081101
Abstract: Recent results of the KASCADE-Grande experiment provided evidence for a mild knee-like structure in the all-particle spectrum of cosmic rays at $E = 10^{16.92 \pm 0.10} \, \mathrm{eV}$, which was found to be due to a steepening in the flux of heavy primary particles. The spectrum of the combined components of light and intermediate masses was found to be compatible with a single power law in the energy range from $10^{16.3} \, \mathrm{eV}$ to $10^{18} \, \mathrm{eV}$. In this paper, we present an update of this analysis by using data with increased statistics, originating both from a larger data set including more recent measurements and by using a larger fiducial area. In addition, optimized selection criteria for enhancing light primaries are applied. We find a spectral feature for light elements, namely a hardening at $E = 10^{17.08 \pm 0.08} \, \mathrm{eV}$ with a change of the power law index from $-3.25 \pm 0.05$ to $-2.79 \pm 0.08$.
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