Detection of 1014-eV iron nuclei in cosmic rays

Sood, R. K.

doi:10.1038/301044a0

Cited by 14 publications

(7 citation statements)

References 8 publications

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“…In the absence of the large light backgrounds due to emission from EAS, it was expected that accurate composition measurements could be made by analysis of the directČerenkov light yields. After a pioneering flight by Sood in 1981 [15], the concept was unexploited until recent efforts by Seckel et al in 1998 [16]. The fundamental challenge in the new approach discussed here is the identification of the DČ light against the much larger background ofČerenkov light produced in the associated EAS.…”

Section: Historymentioning

confidence: 99%

A high resolution method for measuring cosmic ray composition beyond 10 TeV

Kieda

Swordy

Wakely

2001

Astroparticle Physics

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The accurate determination of the elemental composition of cosmic rays at high energies is expected to provide crucial clues on the origin of these particles. Previous direct measurements of composition have been limited by experiment collecting power, resulting in marginal statistics above 10 14 eV, precisely the region where the "knee" of the cosmic-ray energy spectrum is starting to develop. In contrast, indirect measurements using extensive air showers can produce sufficient statistics in this region but generate elemental measurements which have relatively large uncertainties. Here we discuss a technique which has become possible through the use of modern ground-basedČerenkov imaging detectors. We combine a measurement of theČerenkov light produced by the incoming cosmic-ray nucleus in the upper atmosphere with an estimate of the total nucleus energy produced by the extensive air shower initiated when the particle interacts deeper in the atmosphere. The emission regions prior to and after the first hadronic interaction can be separated by an imagingČerenkov system with sufficient angular and temporal resolution. Monte Carlo simulations indicate an expected charge resolution of ∆Z/Z < 5% for incident iron nuclei in the region of the "knee" of the cosmic-ray energy spectrum. This technique also has the intriguing possibility to unambiguously discover nuclei heavier than iron at energies above 10 14 eV. The identification and rejection of background produced by charged particles in ground based gamma-ray telescopes is also discussed.

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Section: Historymentioning

confidence: 99%

A high resolution method for measuring cosmic ray composition beyond 10 TeV

Kieda

Swordy

Wakely

2001

Astroparticle Physics

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“…The central idea of this method is to detect the Cherenkov light emitted by primary cosmic-ray particles (so-called Direct Cherenkov light) from the ground. While DC-light has been measured in the past by balloon experiments [10,11], the measurement from the ground takes advantage of the huge detection area ( 10 5 m 2 ) of IACTs, in principle enabling the extension of spectral and composition measurements up to 1 PeV. Here we review this technique and describe its application to data from H.E.S.S.…”

Section: A Motivationmentioning

confidence: 99%

First ground-based measurement of atmospheric Cherenkov light from cosmic rays

Aharonian¹,

Akhperjanian²,

Bazer‐Bachi³

et al. 2007

Phys. Rev. D

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“…Corrections were also made for hadronic interactions of iron in the atmosphere (estimated 9 %), and for contamination of the iron flux by nuclei with Z = 17-25 (estimated 10%). Sood (1983). We have not reanalyzed Sood's experiment, but have attempted to improve on his pioneering effort in several ways to make our instrument easier to model and the interpretation of the data more certain.…”

Section: Resultsmentioning

confidence: 99%

“…7.-Determinations of the cosmic ray iron flux by other investigators compared to results from PDQ BACH. Sood (1983) pioneered the BACH technique. The JACEE determination (Asakimori et al 1995) is a compilation of data from 12 flights.…”

Section: Resultsmentioning

confidence: 99%

“…By achieving an absolute measurement of the iron flux, relatively free of the uncertainty in particle interaction models, the Balloon Air CHerenkov (BACH) technique can provide an independent calibration for air shower experiments, thus opening a path for composition measurements for energies at and above the knee. This technique was discussed by Sitte (1965) and Gough (1975), and used initially by Sood (1983;Sood and Panettieri, 1981). In this paper we report the result obtained from the initial flight of our developmental balloon payload (PDQ BACH).…”

Section: Introductionmentioning

confidence: 90%

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A measurement of the flux of cosmic ray iron at 5×1013 eV

Clem¹,

Droege²,

Evenson³

et al. 2002

Astroparticle Physics

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We present results from the initial flight of our Balloon Air CHerenkov (BACH) payload. BACH detects air Cherenkov radiation from cosmic ray nuclei as coincident flashes in two optical modules. The flight (dubbed PDQ BACH) took place on April 22, 1998 from Ft. Sumner, New Mexico. During an exposure of 2.75 hours, with a typical threshold energy for iron nuclei of 2.2×10 13 eV, we observed several events cleanly identifiable as iron group nuclei. Analysis of the data yields a new flux measurement that is fully consistent with that reported by other investigations.

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Detection of 1014-eV iron nuclei in cosmic rays

Cited by 14 publications

References 8 publications

A high resolution method for measuring cosmic ray composition beyond 10 TeV

A high resolution method for measuring cosmic ray composition beyond 10 TeV

First ground-based measurement of atmospheric Cherenkov light from cosmic rays

A measurement of the flux of cosmic ray iron at 5×1013 eV

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