Measurements of attenuation and absorption lengths with the KASCADE experiment

Antoni, T.; Apel, W. D.; Badea, Anthony; Bekk, K.; Bercuci, A.; Blümer, H.; Bozdog, H.; Brâncuş, I.M.; Büttner, C.; Chilingarian, A.; Daumiller, K.; Döll, P.; Engel, R.; Engler, J.; Feßler, F.; Gils, H.J.; Glasstetter, R.; Haeusler, R.; Haungs, A.; Heck, D.; Hörandel, J. R.; Iwan, Agnieszka; Kampert, K.‐H.; Klages, H. O.; Maier, G.; Mathes, H.J.; Mayer, H.J.; Milke, J.; Müller, M. A.; Obenland, R.; Oehlschläger, J.; Ostapchenko, S.; Rebel, H.; Risse, M.; Roth, M.; Schatz, G.; Schieler, H.; Scholz, J.; Thouw, T.; Ulrich, H.; Vardanyan, A.; Weindl, A.; Wentz, J.; Wochele, J.; Zabierowski, J.

doi:10.1016/s0927-6505(03)00116-6

Cited by 214 publications

(469 citation statements)

References 13 publications

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“…with the zenith θ, the total atmospheric depth X ground ≈ 1022 g/cm 2 at ground level [140], and the height of the radio emission source h rad = cos θ/κ. The height constant h 0 = RT /M g includes the gas constant R = 8.3145 J/mol/K, the air temperature T , the molar mass M ≈ 0.029 kg/mol, and the gravitational acceleration constant g = 9.81 m/s 2 .…”

Section: Max Reconstruction With Curvature Methodsmentioning

confidence: 99%

Instruments and Methods for the Radio Detection of High Energy Cosmic Rays

Schröder¹

2012

Springer Theses

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Instruments and Methods for the Radio Detection of High Energy Cosmic RaysCosmic rays at energies above 10 15 eV cannot be measured directly due to the low flux. Instead, the properties of the primary cosmic ray particles (arrival direction, energy, mass) have to be reconstructed from measurements of secondary particles forming an air shower. For this, digital radio antenna arrays, like LOPES at the Karlsruhe Institute of Technology (KIT), are a relatively new instrument. The radio emission mainly originates from the deflection of secondary air shower electrons and positrons in the Earth's magnetic field. The radio technique aims at achieving a similar quality in the reconstruction of air shower parameters as the established Cherenkov or fluorescence light detection methods, which in contrast to the radio technique are limited to dark, moonless nights.The present studies aim to advance the air shower radio detection in technological aspects and analysis methods. The developments are mainly applied to LOPES, but also provide a useful set of tools, which will soon be applied on the analysis of first AERA measurements. AERA is a next generation digital radio array at the Pierre Auger Observatory in Argentina. Moreover, this thesis reflects the recent progress in the understanding of the radio emission by air showers. The main results of the studies are:• A new method for time calibration with a reference beacon has been developed.It allows a time resolution of ∼ 1 ns even with large antenna arrays. This is necessary for digital radio interferometry which improves the signal-to-noise ratio and the reconstruction accuracy of the primary particle properties. This method is essential for the measurement of cosmic rays with LOPES, and is going to be applied at AERA.• A per-event comparison of lateral distributions measured with LOPES and REAS3 simulations reflects a significantly improved understanding of the radio emission mechanisms. For the first time a Monte Carlo simulation of the radio emission by air showers can in average reproduce measured data. A detailed investigation of systematic effects was performed to accurately reconstruct LOPES lateral distributions. In particular, a method has been developed to appropriately treat the influence of radio noise on measured lateral distributions.• It is shown that a conical radio wavefront fits LOPES measurements and REAS3 simulations better than a spherical wavefront, which up to now has been assumed for LOPES beamforming analyses. Furthermore, the atmospheric depth of the shower maximum X max can be reconstructed by determining the opening angle of the conical wavefront. However, due to the small lateral extension of LOPES of about 200 m and the high radio background at KIT, the measurement uncertainty (∆X max ≈ 200 g/cm 2 ) is too large for a per-event reconstruction of the primary mass. This will improve at AERA, but could not be examined in detail because of a delay in the construction. • Eine neue Methode zur Zeitkalibration mit einen Rerefenzsender (Beaco...

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Section: Max Reconstruction With Curvature Methodsmentioning

confidence: 99%

Instruments and Methods for the Radio Detection of High Energy Cosmic Rays

Schröder¹

2012

Springer Theses

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“…The LOPES project was initiated in 2001, employing a LOFAR 1 Prototype Station to detect radio emission from EAS in coincidence with the well-established KASCADE [6] particle detector experiment. The goals of the LOPES project are (i) to deliver the "proof of principle" for radio de-tection of cosmic rays with modern interferometric methods, (ii) to study and calibrate the radio emission in the energy regime up to ∼ 10 18 eV, and (iii) to develop and optimise the radio technique for large scale application at ultra-high energies.…”

Section: The Lopes Projectmentioning

confidence: 99%

Radio detection of cosmic ray air showers with LOPES

Huege

Apel

Asch

et al. 2007

Nuclear Physics B - Proceedings Supplements

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In the last few years, radio detection of cosmic ray air showers has experienced a true renaissance, becoming manifest in a number of new experiments and simulation efforts. In particular, the LOPES project has successfully implemented modern interferometric methods to measure the radio emission from extensive air showers. LOPES has confirmed that the emission is coherent and of geomagnetic origin, as expected by the geosynchrotron mechanism, and has demonstrated that a large scale application of the radio technique has great potential to complement current measurements of ultra-high energy cosmic rays. We describe the current status, most recent results and open questions regarding radio detection of cosmic rays and give an overview of ongoing research and development for an application of the radio technique in the framework of the Pierre Auger Observatory.

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“…This is a consequence of neglecting the shower age in formulating the structure functions. Very recently, the KASCADE Collaboration has used an NKG formula to fit muon density distributions [190]. The fits were performed close to the shower core (r < 200 m) with non-conventional values of r M and age parameter, s.…”

Section: Muon Lateral Distribution Functionmentioning

confidence: 99%

High energy physics in the atmosphere: phenomenology of cosmic ray air showers

et al. 2004

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The properties of cosmic rays with energies above 10 6 GeV have to be deduced from the spacetime structure and particle content of the air showers which they initiate. In this review we summarize the phenomenology of these giant air showers. We describe the hadronic interaction models used to extrapolate results from collider data to ultra high energies, and discuss the prospects for insights into forward physics at the LHC. We also describe the main electromagnetic processes that govern the longitudinal shower evolution, as well as the lateral spread of particles. Armed with these two principal shower ingredients and motivation from the underlying physics, we provide an overview of some of the different methods proposed to distinguish primary species. The properties of neutrino interactions and the potential of forthcoming experiments to isolate deeply penetrating showers from baryonic cascades are also discussed. We finally venture into a terra incognita endowed with TeV-scale gravity and explore anomalous neutrino-induced showers.

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Measurements of attenuation and absorption lengths with the KASCADE experiment

Cited by 214 publications

References 13 publications

Instruments and Methods for the Radio Detection of High Energy Cosmic Rays

Instruments and Methods for the Radio Detection of High Energy Cosmic Rays

Radio detection of cosmic ray air showers with LOPES

High energy physics in the atmosphere: phenomenology of cosmic ray air showers

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