Measurements of the muon content of EAS in KASCADE-Grande compared with SIBYLL 2.3 predictions

Arteaga‐Velázquez, J. C.; Rivera-Rangel, D.; Apel, W. D.; Bekk, K.; Bertaina, M.; Blümer, J.; Bozdog, H.; Brâncuş, I.M.; Cantoni, E.; Chiavassa, E.; Cossavella, F.; Daumiller, K.; Souza, Vítor de; Pierro, F. Di; Döll, P.; Engel, R.; Fuhrmann, D.; Gils, H.J.; Glasstetter, R.; Grupen, C.; Haungs, A.; Heck, D.; Hörandel, J.R.; Huber, Daniel; Huege, T.; Kampert, K.H.; Dh, Kang; Klages, H. O.; Link, K.; Łuczak, P.; Mayer, H.J.; Milke, J.; Mitrica, B.; Morello, C.; Oehlschläger, J.; Ostapchenko, S.; Palmieri, N.; Pierog, T.; Rebel, H.; Roth, Markus; Schieler, H.; Schoo, S.; Schröder, Frank G.; Sima, O.; Toma, G. de; Trinchero, G.; Ulrich, H.; Weindl, A.; Wochele, J.; Zabierowski, J.

doi:10.22323/1.301.0316

Cited by 13 publications

(11 citation statements)

References 5 publications

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“…In this energy region, the shape of the all-particle spectrum has been measured with high statistical precision. Measurements of the flux spectra for primary mass groups at-and-above the second knee have been performed by several collaborations [82,110,141,142]. The second-knee corresponds to a point in the spectrum where the average nuclear mass is relatively heavy, mostly CNO-like or heavier, but where this flux of heavy elements exhibits a softening.…”

Section: Understanding the Transition To Extragalactic Sourcesmentioning

confidence: 99%

Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers

Coleman,

Eser,

Mayotte

et al. 2022

Preprint

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Pin down the shower energy observable to use μ as a composition-only Reduce hadronic uncertainties interaction model E threshold (TBD) Other messengers Galactic * μ / em separation † * depending on analysis progress † depending on detector configuration• At least one next-generation experiment needs to be able to make high-precision measurements to explore new particle physics and measure particle rigidity on an event-by-event basis. Of the planned next-generation experiments, GCOS is the best positioned to meet this recommendation.• As a complementary effort, experiments with sufficient exposure ( 5 × 10 5 km 2 sr yr) are needed to search for Lorentz-invariance violation (LIV), SHDM, and other BSM physics at the Cosmic and Energy Frontiers, and to identify UHECR sources at the highest energies.• Full-sky coverage with low cross-hemisphere systematic uncertainties is critical for astrophysical studies. To this end, next generation experiments should be space-based or multi-site. Common sites between experiments are encouraged.• Based on the productive results from inter-collaboration and inter-disciplinary work, we recommend the continued progress/formation of joint analyses between experiments and with other intersecting fields of research (e.g., magnetic fields).• The UHECR community should continue its efforts to advance diversity, equity, inclusion, and accessibility. It also needs to take steps to reduce its environmental impacts and improve open access to its data to reduce the scientific gap between countries.vi

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Section: Understanding the Transition To Extragalactic Sourcesmentioning

confidence: 99%

Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers

Coleman,

Eser,

Mayotte

et al. 2022

Preprint

Self Cite

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“…Therefore, only the H and He spectra are compared directly as the other groups are strongly correlated. Kascade-Grande [49] results are using a three component fit of H, HeCNO, and Heavy groups using Sibyll 2.3. Therefore, only the H and Heavy spectra are compared, as the HeCNO group cannot be deconvoluted into a He and CNO part.…”

Section: Acknowledgmentsmentioning

confidence: 99%

Cosmic ray spectrum and composition from PeV to EeV using 3 years of data from IceTop and IceCube

Aartsen¹,

Ackermann²,

Adams³

et al. 2019

Phys. Rev. D

118

109

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“…Therefore only the H and He spectra are compared directly as the other groups are strongly correlated. Kascade-Grande [46] results are using a 3 component fit of H, HeCNO and Heavy groups using Sibyll 2.3. Therefore only the H and Heavy spectra are compared, as the HeCNO group cannot be deconvoluted into a He and CNO part.…”

Section: Discussionmentioning

confidence: 99%

Cosmic Ray Spectrum and Composition from PeV to EeV Using 3 Years of Data From IceTop and IceCube

2019

Preprint

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We report on measurements of the all-particle cosmic ray energy spectrum and composition in the PeV to EeV energy range using three years of data from the IceCube Neutrino Observatory. The IceTop detector measures cosmic ray induced air showers on the surface of the ice, from which the energy spectrum of cosmic rays is determined by making additional assumptions about the mass composition. A separate measurement is performed when IceTop data are analyzed in coincidence with the high-energy muon energy loss information from the deep in-ice IceCube detector. In this measurement, both the spectrum and the mass composition of the primary cosmic rays are simultaneously reconstructed using a neural network trained on observables from both detectors.

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Measurements of the muon content of EAS in KASCADE-Grande compared with SIBYLL 2.3 predictions

Cited by 13 publications

References 5 publications

Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers

Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers

Cosmic ray spectrum and composition from PeV to EeV using 3 years of data from IceTop and IceCube

Cosmic Ray Spectrum and Composition from PeV to EeV Using 3 Years of Data From IceTop and IceCube

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