Status of the Yakutsk Air Shower Array and Future Plans
- Elementary Particles and Fields/Experiment
- Published: 29 December 2021
- Volume 84 , pages 893–906, ( 2021 )
Cite this article
- A. K. Alekseev 1 ,
- E. A. Atlasov 1 ,
- N. G. Bolotnikov 1 ,
- A. V. Bosikov 1 ,
- N. A. Dyachkovskiy 1 ,
- N. S. Gerasimova 1 ,
- A. V. Glushkov 1 ,
- A. A. Ivanov 1 ,
- O. N. Ivanov 1 ,
- D. N. Kardashevsky 1 ,
- I. A. Kellarev 1 ,
- S. P. Knurenko 1 ,
- A. D. Krasilnikov 1 ,
- A. N. Krivenkov 1 ,
- I. V. Ksenofontov 1 ,
- L. T. Ksenofontov 1 ,
- K. G. Lebedev 1 ,
- S. V. Matarkin 1 ,
- V. P. Mokhnachevskaya 1 ,
- E. V. Nikolaeva 1 ,
- N. I. Neustroev 1 ,
- I. S. Petrov 1 ,
- N. D. Platonov 1 ,
- A. S. Proshutinsky 1 ,
- A. V. Saburov 1 ,
- I. Ye. Sleptsov 1 ,
- G. G. Struchkov 1 ,
- L. V. Timofeev 1 &
- B. B. Yakovlev 1
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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.
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This report was made within the framework of the research project AAAA-A21-121011990011-8 curated by the Ministry of Science and Higher Education of the Russian Federation.
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A. K. Alekseev, E. A. Atlasov, N. G. Bolotnikov, A. V. Bosikov, N. A. Dyachkovskiy, N. S. Gerasimova, A. V. Glushkov, A. A. Ivanov, O. N. Ivanov, D. N. Kardashevsky, I. A. Kellarev, S. P. Knurenko, A. D. Krasilnikov, A. N. Krivenkov, I. V. Ksenofontov, L. T. Ksenofontov, K. G. Lebedev, S. V. Matarkin, V. P. Mokhnachevskaya, E. V. Nikolaeva, N. I. Neustroev, I. S. Petrov, N. D. Platonov, A. S. Proshutinsky, A. V. Saburov, I. Ye. Sleptsov, G. G. Struchkov, L. V. Timofeev & B. B. Yakovlev
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Alekseev, A.K., Atlasov, E.A., Bolotnikov, N.G. et al. Status of the Yakutsk Air Shower Array and Future Plans. Phys. Atom. Nuclei 84 , 893–906 (2021). https://doi.org/10.1134/S1063778821130020
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DOI : https://doi.org/10.1134/S1063778821130020
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The Energy Spectrum Observed by the AGASA Experiment and the Spatial Distribution of the Sources of Ultra-High-Energy Cosmic Rays
Gustavo A. Medina-Tanco 1
Published 1998 December 15 • © 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. The Astrophysical Journal , Volume 510 , Number 2 Citation Gustavo A. Medina-Tanco 1999 ApJ 510 L91 DOI 10.1086/311814
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1 Instituto Astronômico e Geofísico, Universidade de São Paulo, Caixa Postal 9638, São Paulo, SP 01065-970, Brasil; and Department of Physics and Astronomy, University of Leeds, Leeds LS2 9JT, England, UK
- Received 1998 September 23
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- Published 1998 December 15
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Seven and a half years of continuous monitoring of giant air showers triggered by ultra-high-energy cosmic rays have been summarized recently by the AGASA collaboration. The resulting energy spectrum indicates clearly that the cosmic-ray spectrum extends well beyond the Greisen-Zatsepin-Kuzmin (GZK) cutoff at ~5 × 10 19 eV. Furthermore, despite the small-number statistics involved, some structure in the spectrum may be emerging. Using numerical simulations, it is demonstrated in the present work that these features are consistent with a spatial distribution of sources that follows the distribution of luminous matter in the local universe. Therefore, from this point of view, there is no need for a second high-energy component of cosmic rays dominating the spectrum beyond the GZK cutoff.
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Results from AGASA experiment in the extremely high energy region
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Motohiko Nagano; Results from AGASA experiment in the extremely high energy region. AIP Conf. Proc. 15 June 1998; 433 (1): 76–86. https://doi.org/10.1063/1.56148
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Recent results on primary cosmic rays of energies above 1×10 19 eV observed by the Akeno Giant Air Shower Array (AGASA) are summarized. It is likely that extremely high energy cosmic rays are from diffuse sources distributed isotropically in the universe. However, there are cosmic rays of energies in excess of the predicted cutoff energy and some fraction of cosmic rays beyond 4×10 19 eV seem to come nearby sources composing double events within a limited space angle.
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- DOI: 10.1086/311814
- Corpus ID: 121754057
The Energy Spectrum Observed by the AGASA Experiment and the Spatial Distribution of the Sources of Ultra-High-Energy Cosmic Rays
- G. Medina-Tanco
- Published 10 January 1999
- The Astrophysical Journal Letters
17 Citations
The high-energy cosmic ray spectrum from relic particle decay, a possible nearby origin for the highest-energy events observed, status and prospects of the ultrahigh energy cosmic rays, particle and astrophysical aspects of ultra-high energy cosmic rays, cosmic magnetic fields from the perspective of ultra-high-energy cosmic rays propagation, the greisen–zatzepin–kuzmin feature in our neighborhood of the universe, ultrahigh energy cosmic rays: the state of the art before the auger observatory, cosmic rays from remnants of quasars.
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Ultra-high Energy Cosmic Rays: From GeV to ZeV
Ultrahigh-energy cosmic-ray propagation in the galaxy: clustering versus isotropy, 36 references, energy spectrum of ultra-high energy cosmic rays with extra-galactic origin, extension of the cosmic-ray energy spectrum beyond the predicted greisen-zatsepin-kuz'min cutoff, detection of a cosmic ray with measured energy well beyond the expected spectral cutoff due to cosmic microwave radiation, the highest energy cosmic rays, the extremely high energy cosmic rays, non-diffusive propagation of ultra high energy cosmic rays, ultrahigh energy cosmic rays without greisen-zatsepin-kuzmin cutoff, cosmological origin for cosmic rays above 1019 ev, the effect of highly structured cosmic magnetic fields on ultra-high-energy cosmic-ray propagation, ultra high energy cosmic rays, related papers.
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IMAGES
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The results from AGASA were used to calculate the energy spectrum and anisotropy of cosmic rays. The results helped to confirm the existence of ultra-high energy cosmic rays (> 5 × 10 19 eV), such as the so-called "Oh-My-God" particle that was observed by the Fly's Eye experiment run by the University of Utah.The Telescope Array, a merger of the AGASA and High Resolution Fly's Eye (HiRes ...
This array is called the Akeno Giant Air Shower Array (AGASA) . AGASA covers an area of about 100 km2 and consists of 111 detectors on the ground (surface detectors) and 27 detectors under absorbers (muon detectors). Each surface detector is placed with a nearest-neighbor separation of about 1 km and the detectors are sequentially connected ...
The Telescope Array project is an international collaboration involving research and educational institutions in Japan, The United States, Russia, South Korea, and Belgium. [1] The experiment is designed to observe air showers induced by ultra-high-energy cosmic ray using a combination of ground array and air-fluorescence techniques. It is located in the high desert in Millard County, Utah ...
It is one of the longest running experiments that register the flux of the ultra-high energy CRs (UHECR): it has been continuously operating since 1973. From the very beginning it was created as a complex instrument, capable of measuring several EAS components with different types of detectors. ... , and AGASA . (d) Same as in panel (c) but ...
Here, we will discuss the results obtained by AGASA, the Akeno Giant Air Shower Array, covering over 100km2 area in operation at Akeno village about 130km west of Tokyo. 2 The Highest Energy Cosmic Rays Figure 1 shows the energy spectrum above 1018·5 eV observed by AGASA experiment (Takeda et al. 1998, Hayashida et al 2000). For reference, we ...
In the AGASA experiment, pulse widths of all incident particles are recorded and their PWD is stored in the memory as shown in Fig. 1, and then t 1 is determined in every RUN. Fig. 4(a) shows the time variation of t 1 for a typical detector over 12 years of operation. There is a clear seasonal variation with a ±3% fluctuation, but this ...
Summary The AGASA experiment had been operated since 1990 and was finished in January 2004 having detected about 1000 UHECRs above 10 19 eV. With elaborate simulations and experimental studies, the data quality has been well confirmed. Through 14-year operation, we have obtained many important findings to deepen our understanding of the highest ...
Abstract: (Elsevier) Through a 14-year operation of the Akeno Giant Air Shower Array (AGASA), we detected about 1000 UHECRs above 10 19 eV including eleven events above 10 20 eV. The data indicate that the cosmic ray spectrum extends well beyond the predicted Greisen-Zatsepin-Kuzmin cutoff.
The results from both experiments would meet except for the super-GZK part if the energy scale of HiRes were pushed up by ∼ 30% [29]. Surface array experiment such as AGASA is even more easily and preciously understood. It is suggested that the energy of the spectral change, ankle could be a calibration point.
The energy spectrum measured by the AGASA experiment (black dots) [21] is compared with the calculations (green squares). The blue line is normalized to the Auger data[7] while the black ...
Seven and a half years of continuous monitoring of giant air showers triggered by ultra-high-energy cosmic rays have been summarized recently by the AGASA collaboration. The resulting energy spectrum indicates clearly that the cosmic-ray spectrum extends well beyond the Greisen-Zatsepin-Kuzmin (GZK) cutoff at ~5 × 10 19 eV. Furthermore ...
Using data from more than ten-years of observations with the Akeno Giant Air Shower Array (AGASA), we published a result that the energy spectrum of ultra-high energy cosmic rays extends beyond the cutoff energy predicted by Greisen, and Zatsepin and Kuzmin. In this paper, we reevaluate the energy determination method used for AGASA events with respect to the lateral distribution of shower ...
A cosmic ray—an atomic nucleus hurtling through space—struck a detector in an array called the Volcano Ranch experiment with an energy of 10 20 electronvolts, or 100 ... near Tokyo, bagged about a dozen more particles with energies of about 200 EeV. The AGASA results galvanized astrophysicists into building a much bigger detector optimized ...
In this experiment, the total number of electrons, known as the shower size Ne, was used as an energy estimator. The relation between this energy spectrum and the AGASA energy spectrum is discussed in §4. 2 Densities measured by scintillation detectors The AGASA array consists of plastic scintillators of 2.2m2 area, and the
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Seven and a half years of continuous monitoring of giant air showers triggered by ultra high-energy cosmic rays have been recently summarized by the AGASA collaboration. The resulting energy spectrum indicates clearly that the cosmic ray spectrum extends well beyond the Greisen-Zatsepin-Kuzmin (GZK) cut-off at $\\sim 5 \\times 10^{19}$ eV. Furthermore, despite the small number statistics ...
The data acquisition system of the Akeno Giant Air Shower Array (AGASA) is described. The AGASA array covers an area of about 100 km 2 and has been operated since 1990 to study the origin of extremely high energy cosmic rays. In the early stage of our experiment, AGASA was divided into four sub-arrays called branches for topographical reasons so that air showers were observed independently at ...
Abstract: The Telescope Array (TA) Experiment is the largest ultra-high energy cosmic ray detector in the northern hemisphere. The Telescope Array is a follow up to the High Resolution Fly s Eye and AGASA experiments. It is located near Delta, Utah, about 200 kilometers southwest of SaltLake City, Utah, USA.The detector consists of 507 three square
Seven and a half years of continuous monitoring of giant air showers triggered by ultra-high-energy cosmic rays have been summarized recently by the AGASA collaboration. The resulting energy spectrum indicates clearly that the cosmic-ray spectrum extends well beyond the Greisen-Zatsepin-Kuzmin (GZK) cutoff at ~5 × 1019 eV. Furthermore, despite the small-number statistics involved, some ...
The AGASA energy spectrum in the highest energy region, which is adjusted to the one of the 1 km 2 array at Akeno [11] 2 are compared with the spectra from the Haverah Park [12], Yakutsk [13] and stereo Fly's Eye [14] experiments in Fig. 1.All four spectra agree with one another within ±15% in energy.
5.1 Definition of density used in Akeno/AGASA experiment. In the AGASA experiment, a scintillator of 5 cm thickness is used to detect particles on the surface. The scintillator is placed inside an enclosure made of iron of 1.5 ∼ 2 mm thickness and the detector is in a hut whose roof is made of an iron plate of.
AirShowerArray(AGASA)inJapanandtheHigh Resolution Fly's Eye (HiRes) in the USA. The AGASA experiment published an energy spectrum which does not exhibit the GZK cutoff in 1998 [2]. The spectrum above 1019 eV is well described by E−2.78 distribution, and a total of 6 events was observed above 1020 eV with an ex-posure of 0.83 × 103 km2 sr ...
In this work the ultra high energy cosmic ray events recorded by the AGASA experiment are analyzed. With detailed simulations of the extensive air showers initiated by photons, the probabilities are determined of the photonic origin of the 6 AGASA events for which the muon densities were measured and the reconstructed energies exceeded 10 20 eV. On this basis a new, preliminary upper limit on ...