Lateral distribution of the radio signal in extensive air showers measured with LOPES

Apel, W. D.; Arteaga, J.C.; Asch, T.; Badea, Anthony; Bähren, L.; Bekk, K.; Bertaina, M.; Biermann, P. L.; Blümer, J.; Bozdog, H.; Brancus, I. M.; Brüggemann, M.; Buchholz, P.; Buitink, S.; Cantoni, E.; Чиавасса, А.; Cossavella, F.; Daumiller, K.; Souza, V. de; Pierro, F. Di; Döll, P.; Engel, R.; Falcke, H.; Finger, M.; Fuhrmann, D.; Gemmeke, H.; Ghia, P. L.; Glasstetter, R.; Grupen, C.; Haungs, A.; Heck, D.; Hörandel, J. R.; Horneffer, A.; Huege, T.; Isar, P. G.; Kampert, K.‐H.; Kang, D.; Kickelbick, D.; Krömer, O.; Kuijpers, J.; Lafèbre, S.; Łuczak, P.; Ludwig, M.; Mathes, H. J.; Mayer, H.J.; Melissas, M.; Mitrica, B.; Morello, C.; Navarra, G.; Nehls, S.; Nigl, A.; Oehlschläger, J.; Over, S.; Palmieri, N.; Petcu, M.; Pierog, T.; Rautenberg, J.; Rebel, H.; Roth, M.; Sǎftoiu, A.; Schieler, H.; Schmidt, A.; Schröder, Frank G.; Sima, O.; Singh, K.; Toma, G.; Trinchero, G.; Ulrich, H.; Weindl, A.; Wochele, J.; Wommer, M.; Zabierowski, J.; Zensus, J. A.

doi:10.1016/j.astropartphys.2009.09.007

Cited by 77 publications

(53 citation statements)

References 19 publications

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“…Thus, we have decided to use an exponential LDF with an amplitude and a slope parameter, as already in Refs. [24,25] -in particular since a power law as alternative 2-parameter LDF has been shown to be inappropriate for LOPES events [24].…”

Section: Lateral Distribution Function (Ldf)mentioning

confidence: 99%

“…[24]: First, we use the amplitude at an axis distance of 100 m as fit parameter instead of the amplitude at the shower core, since 100 m is close to the mean axis distance of about 120 m and close to the distance where least fluctuations due to the primary particle type are expected for LOPES (70 − 90 m) [49]. This reduces the uncertainty of the amplitude fit parameter while still describing the same physics.…”

Section: Lateral Distribution Function (Ldf)mentioning

confidence: 99%

“…Although a scale uncertainty is not important when comparing several LOPES events with each other (as in Ref. [24]), it is crucial when comparing LOPES events with other experiments or simulations. In particular, the scale uncertainty limits the testing power whether a theoretical model can predict the absolute amplitude correctly.…”

Section: Amplitude Calibrationmentioning

confidence: 99%

“…The lateral distribution of the radio signal is the variation of the radio amplitude ǫ with the distance to air shower axis d. It has already been studied with LOPES [24,25] and other experiments (e.g., CODALEMA [12]), and already it was compared to simulations [26], however, only for single events or with a limited statistics. These limited studies had been sufficient to show that earlier models, not yet including the refractive index of the air, could not fully reproduce the measurements.…”

Section: Introductionmentioning

confidence: 99%

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Comparing LOPES measurements of air-shower radio emission with REAS 3.11 and CoREAS simulations

Apel

Arteaga‐Velázquez

Bähren

et al. 2013

Astroparticle Physics

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Comparing LOPES measurements of air-shower radio emission with REAS 3.11 and CoREAS simulations AbstractCosmic ray air showers emit radio pulses at MHz frequencies, which can be measured with radio antenna arrays -like LOPES at the Karlsruhe Institute of Technology in Germany. To improve the understanding of the radio emission, we test theoretical descriptions with measured data. The observables used for these tests are the absolute amplitude of the radio signal, and the shape of the radio lateral distribution. We compare lateral distributions of more than 500 LOPES events with two recent and public Monte Carlo simulation codes, REAS 3.11 and CoREAS (v 1.0). The absolute radio amplitudes predicted by REAS 3.11 are in good agreement with the LOPES measurements. The amplitudes predicted by CoREAS are lower by a factor of two, and marginally compatible with the LOPES measurements within the systematic scale uncertainties. In contrast to any previous versions of REAS, REAS 3.11 and CoREAS now reproduce the shape of the measured lateral distributions correctly. This reflects a remarkable progress compared to the situation a few years ago, and it seems that the main processes for the radio emission of air showers are now understood: The emission is mainly due to the geomagnetic deflection of the electrons and positrons in the shower. Less important but not negligible is the Askaryan effect (net charge variation). Moreover, we confirm that the refractive index of the air plays an important role, since it changes the coherence conditions for the emission: Only the new simulations including the refractive index can reproduce rising lateral distributions which we observe in a few LOPES events. Finally, we show that the lateral distribution is sensitive to the energy and the mass of the primary cosmic ray particles.

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Section: Lateral Distribution Function (Ldf)mentioning

confidence: 99%

Section: Lateral Distribution Function (Ldf)mentioning

confidence: 99%

Section: Amplitude Calibrationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Comparing LOPES measurements of air-shower radio emission with REAS 3.11 and CoREAS simulations

Apel

Arteaga‐Velázquez

Bähren

et al. 2013

Astroparticle Physics

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“…Therefore, the direct estimation of both E EW 0 and d 0 for each event is not possible. Nevertheless, it is still possible to obtain an estimation of the electric field value E EW 0 , assuming the parameter d 0 to be 150 m as suggested by the CODALEMA [29] and LOPES [30] experiments. We also have to rescale E EW 0 to a normalized value depending on the incoming arrival direction and the geomagnetic field n × B.…”

Section: Correlation Between Shower Energy and Electric Fieldmentioning

confidence: 99%

Results of a self-triggered prototype system for radio-detection of extensive air showers at the Pierre Auger Observatory

et al. 2012

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We describe the experimental setup and the results of RAuger, a small radio-antenna array, consisting of three fully autonomous and self-triggered radio-detection stations, installed close to the center of the Surface Detector (SD) of the Pierre Auger Observatory in Argentina. The setup has been designed for the detection of the electric field strength of air showers initiated by ultra-high energy cosmic rays, without using an auxiliary trigger from another detection system. Installed in December 2006, RAuger was terminated in May 2010 after 65 registered coincidences with the SD. The sky map in local angular coordinates (i.e., zenith and azimuth angles) of these events reveals a strong azimuthal asymmetry which is in agreement with a mechanism dominated by a geomagnetic emission process. The correlation between the electric field and the energy of the primary cosmic ray is presented for the first time, in an energy range covering two orders of magnitude between 0.1 EeV and 10 EeV. It is demonstrated that this setup is relatively more sensitive to inclined showers, with respect to the SD. In addition to these results, which underline the potential of the radio-detection technique, important information about the general behavior of self-triggering radio-detection systems has been obtained. In particular, we will discuss radio self-triggering under varying local electric-field conditions. * Authors are listed on the following pages.

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Indirect Detection of Cosmic Rays

Engel

Schmidt

2021

Handbook of Particle Detection and Imaging

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Lateral distribution of the radio signal in extensive air showers measured with LOPES

Cited by 77 publications

References 19 publications

Comparing LOPES measurements of air-shower radio emission with REAS 3.11 and CoREAS simulations

Comparing LOPES measurements of air-shower radio emission with REAS 3.11 and CoREAS simulations

Results of a self-triggered prototype system for radio-detection of extensive air showers at the Pierre Auger Observatory

Indirect Detection of Cosmic Rays

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