The energy spectrum of cosmic rays above 10^15 eV as derived from air Cherenkov light measurements in Yakutsk

Abstract

The Yakutsk array observes the Cherenkov light emitted by UHECR in atmosphere. Recently, an autonomous subarray is added consisting of photomultipliers to measure the showers in the knee region. Our aim is to analyze the combined data set in order to derive the cosmic ray spectrum in the energy range as wide as possible using the same technique. The advantage of the air Cherenkov light measurement is the model independent estimation of the EAS primary energy using the total light flux emitted in the atmosphere. A set of the light lateral distributions observed in the extended energy range is presented also.

11 pages, 5 figures, submitted to Nuclear Physics B (Proceedings Supplements)

Cited by in corpus (12)

• Spectrum of cosmic rays, produced in supernova remnants
• The spectrum features of UHECRs below and surrounding GZK
• Measuring extensive air showers with Cherenkov light detectors of the Yakutsk array: The energy spectrum of cosmic rays
• Cosmic Rays: The Second Knee and Beyond
• Do Ultrahigh Energy Cosmic Rays Come from Active Galactic Nuclei and Fermi $\gamma$-ray Sources?
• Recent results from Yakutsk experiment: development of EAS, energy spectrum and primary particle mass composition in the energy region of 10^15-10^19 eV
• Air Cherenkov Methods in Cosmic Rays: A Review and Some History
• Cosmic ray spectrum by energy scattered by EAS particles in the atmosphere and galactic model
• Zenith angle distribution of cosmic ray showers measured with the Yakutsk array and its application to analysis of arrival directions in equatorial coordinates
• Measuring temporal characteristics of the Cherenkov radiation signal from extensive air showers of cosmic rays with a wide field-of-view telescope addendum to the Yakutsk array
• On UHECR energy estimation algorithms based on the measurement of electromagnetic component parameters in EAS
• Prospects for discovery of physics beyond the Standard Model at the Pierre Auger Observatory