Depth of shower maximum and mass composition of cosmic rays from 50 PeV to 2 EeV measured with the LOFAR radio telescope

Corstanje, A.; Buitink, S.; Falcke, H.; Hare, B. M.; Hörandel, J. R.; Huege, T.; Krampah, G. K.; Mitra, P.; Mulrey, K.; Nelles, A.; Pandya, Hershal; Rachen, J. P.; Scholten, Olaf; Veen, S. ter; Thoudam, Satyendra; Trinh, Gia; Winchen, T.

doi:10.1103/physrevd.103.102006

Cited by 36 publications

(39 citation statements)

References 43 publications

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“…Recent advancements such as from including time-varying atmospheric conditions [836] into the simulations have improved X max resolutions further, circumventing the uncertainties previously encountered in the averaged LDF parametrization models for X max . Results by Tunka-Rex [181], LOFAR [180], and AERA [179] have shown resolutions up to 15 − 25 g/cm 2 can be achieved with similar implementations of this method.…”

Section: Radio Energymentioning

confidence: 95%

“…The low-energy enhancements TALE [142] of TA and HEAT [53] of Auger measure the X max of FD events which reach their points of maximum shower development high in the atmosphere. The radio arrays AERA [179], LOFAR [180], Tunka-Rex [181],…”

Section: Primary Composition: 100 Pev-1 Eevmentioning

confidence: 99%

“…Pierre Auger Observatory: FD [53], SD [192], RD (AERA) [179]; Telescope Array: FD [74] ( X max and σ(X max ) are corrected for reconstruction and detector biases same as was done in Ref. [2] except here there is no correction of the energy scale), Cherenkov (TALE) [142]; Yakutsk: Cherenkov [178], RD [182]; Tunka: Cherenkov [177], RD [181]; LOFAR [180]. Systematic uncertainties of the FD measurements at 10 18.5 eV are indicated for the Pierre Auger (red arrows) and Telescope Array (blue arrows) data.…”

Section: Primary Composition Above 1 Eevmentioning

confidence: 99%

“…Efforts will be made to further reduce the uncertainty on the antenna calibration in the future which brings in reach a precision of individual events as well as an absolute accuracy for the energy of better than 10 %. LOFAR [180], Tunka-Rex [181], and Yakutsk-Radio [182]) and compared to world data (Auger FD [53] and SD [192], HiRes/MIA [826], TA [74], TALE [142], Tunka-133 [177], and Yakutsk [178]).…”

Section: Radio Energymentioning

confidence: 99%

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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: Radio Energymentioning

confidence: 95%

Section: Primary Composition: 100 Pev-1 Eevmentioning

confidence: 99%

Section: Primary Composition Above 1 Eevmentioning

confidence: 99%

Section: Radio Energymentioning

confidence: 99%

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

Coleman,

Eser,

Mayotte

et al. 2022

Preprint

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“…where Tunka-133 [22] (crosses), TA [25] (empty diamonds), PAO [24] (grey asterisks) and LOFAR [54] (grey circles). Points denoted as "muons" are results of direct measurements of muon fluxes in EAS:…”

Section: Muon Component Of Extensive Air Showersmentioning

confidence: 99%

Status of the Yakutsk air shower array and future plans

Alekseev,

Atlasov,

Bolotnikov

et al. 2021

Preprint

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The Yakutsk Extensive Air Shower Array has been continuously operating for more than 50 years (since 1970) and up until recently it has been one of world's largest ground-based instruments aimed at studying the properties of cosmic rays in the ultra-high energy domain. In this report we discuss results recently obtained at the array -on cosmic rays energy spectrum, mass composition and directional anisotropy -and how they fit into the world data. Special attention is paid to the measurements of muonic component of extensive air showers. Theoretical results of particle acceleration at shocks are also briefly reviewed. Future scientific and engineering plans on the array modernization are discussed. I. INTRODUCTIONThe only way to study the properties of cosmic rays (CR) with energies above ∼ 10 15 eV is by registering extensive air showers (EAS) -cascades of secondary particles produced by high-energy CRs hitting Earth's atmosphere. On one hand by studying the EAS properties one can investigate hadron interactions at energies unreachable for terrestrial particle acceleration technology. On the other hand -EAS method provides the basis for obtaining crucial information on primary CR properties: their energy spectrum, mass composition and distribution of arrival directions on the celestial sphere. Hence, EAS study is a dedicated area of CR physics at the intersection of astrophysics and nuclear physics.

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