Measurement of Light Emission from Remote Cosmic-Ray Air Showers

Bergeson, H. E.; Cassiday, G. L.; Chiu, Ting‐Wai; Cooper, D. A.; Elbert, J. W.; Loh, E. C.; Steck, D.; West, William B.; Linsley, J.; Mason, G. W.

doi:10.1103/physrevlett.39.847

Cited by 47 publications

(46 citation statements)

References 3 publications

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“…Neither the Cornell nor the Japanese sites were climatically suitable for exploiting the promise of the method, but the challenge was taken up by Keuffel's group at the University of Utah. In 1976, at Volcano Ranch, unambiguous detection of fluorescent emission from showers, in coincidence with a ground array, was established (Bergeson et al, 1977). This success led to the development of the very successful Fly's Eye instrument (Baltrusaitis, Cady, et al, 1985a).…”

Section: Historical Backgroundmentioning

confidence: 99%

Observations and implications of the ultrahigh-energy cosmic rays

2000

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The authors define ''ultrahigh-energy cosmic rays'' (UHECRs) as those cosmic rays with energies above 10 18 eV. It had been anticipated that there would be a cutoff in the energy spectrum of primary cosmic rays around 6ϫ10 19 eV induced by the interaction of the particles with the 2.7-K primordial photons. However, recent experimental data have established that particles exist with energies greatly exceeding this. It follows that the sources of such particles are probably nearby, on a cosmological scale. However, although the trajectories of such energetic particles through the galactic and intergalactic magnetic fields may be nearly rectilinear, no astronomical sources have as yet been identified. This is the enigma of the highest-energy cosmic rays. The paper reviews the history of research in this energy regime and critically assesses the observational results on the energy spectrum, arrival directions, and composition of the primary cosmic rays based on observations made by six experiments. The detection methods currently available are described. Special techniques have been developed as particles of 10 20 eV or higher occur at a rate of only about 1 per km 2 per century. Errors in measurement are given particular attention. The authors also review the theoretical predictions for a number of candidate sources of cosmic rays beyond the predicted cutoff. Finally, the four major projects planned to address the question of the origin of UHECRs are briefly described. CONTENTS

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Section: Historical Backgroundmentioning

confidence: 99%

Observations and implications of the ultrahigh-energy cosmic rays

2000

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“…19 For example, an explanation of the apparent absence of a counterjet in Cen A via relativistic beaming suggests that the angle of the visible jet axis with respect to the line of sight is at most 36 • [236], which could lead to a doubling of the hot spot radius. It should be remarked that for a distance of 3.4 Mpc, the extent of the entire source has a reasonable size even with this small angle.…”

Section: Radiogalaxiesmentioning

confidence: 99%

“…The actual size can be larger by a factor ∼ 2 because of uncertainties in the angular projection of this region along the line of sight. 19 Then, if the magnetic field of the hot spot is confined to the visible region, the limiting energy imposed by the Hillas' criterion is E max ∼ 10 20.6 eV.…”

Section: Radiogalaxiesmentioning

confidence: 99%

“…The fluorescence technique has so far been implemented only in the Dugway desert (Utah). Following a successful trial at Volcano Ranch [19] the group from the University of Utah built a device containing two separated Fly's Eyes [20,21]. The two-eye configuration monitored the sky from 1986 until 1993.…”

Section: There's Something About Cosmic Ray Observations a Experimentioning

confidence: 99%

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Astrophysical origins of ultrahigh energy cosmic rays

2004

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In the first part of this review we discuss the basic observational features at the end of the cosmic ray energy spectrum. We also present there the main characteristics of each of the experiments involved in the detection of these particles. We then briefly discuss the status of the chemical composition and the distribution of arrival directions of cosmic rays. After that, we examine the energy losses during propagation, introducing the Greisen-Zaptsepin-Kuzmin (GZK) cutoff, and discuss the level of confidence with which each experiment have detected particles beyond the GZK energy limit. In the second part of the review, we discuss astrophysical environments able to accelerate particles up to such high energies, including active galactic nuclei, large scale galactic wind termination shocks, relativistic jets and hot-spots of Fanaroff-Riley radiogalaxies, pulsars, magnetars, quasar remnants, starbursts, colliding galaxies, and gamma ray burst fireballs. In the third part of the review we provide a brief summary of scenarios which try to explain the super-GZK events with the help of new physics beyond the standard model. In the last section, we give an overview on neutrino telescopes and existing limits on the energy spectrum and discuss some of the prospects for a new (multi-particle) astronomy. Finally, we outline how extraterrestrial neutrino fluxes can be used to probe new physics beyond the electroweak scale. Solicited Review Article Prepared for Reports on Progress in Physics 1 PREFACEReviewing cosmic ray physics is a risky business. Theoretical models continue to appear at an amazing rate, both in the astrophysical and more exotic domains. We warn the reader: we do not (nor we could) intend to make an homogeneous coverage of all the ideas of our fellow colleagues. Reading differently focused reviews on the issue (quoted here along the way) is, in our view, the best approach to such a wide topic of research.2 Contents

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“…More precisely measurement are required to explore the UHECR physic. Building a large scale observation, such as Pierre Auger Observtory [4], and Telescope Array Observtory [5][6][7], is the most direct stratagy to understand the UHECR with the low flux. Systematic uncertainties of energy scale reconstruction include several parts: 1) fluorescence yield, 2) detector calibration, 3) atmospheric transmission and so on.…”

Section: Ultra-high Energy Cosmic Raysmentioning

confidence: 99%

Geant4 simulation of sFLASH experiment

Huang¹

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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The goal of Super Fluorescence Air SHower (sFLASH) is to reduce the current fluorescence yield systematic uncertainty to improve energy measurement of ultra-high energy cosmic rays. The experiment was performed at SLAC National Accelerator Laboratory to measure the air fluorescence yield from extensive air showers. A set of alumina bricks is placed in front of the beam pipe as the target to generate a cascade in the bricks. When the charged particles of cascade escape from the target, they excite the air molecules and emit the fluorescence. Several photon multipliers collect the fluorescence in the dark room to estimate the fluorescence yield. In this simulation, the proper geometry of this experiment is built with Geant4, which is the simulation toolkit for high energy particle interactions.

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Measurement of Light Emission from Remote Cosmic-Ray Air Showers

Cited by 47 publications

References 3 publications

Observations and implications of the ultrahigh-energy cosmic rays

Observations and implications of the ultrahigh-energy cosmic rays

Astrophysical origins of ultrahigh energy cosmic rays

Geant4 simulation of sFLASH experiment

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