Techniques of the FLASH thin target experiment

Abbasi, Rasha; Abu‐Zayyad, T.; Belov, K.; Belz, J. W.; Bergman, D. R.; Cao, Zhen; Chang, Feng‐Chih; Chen, C. C.; Chen, C. W.; Chen, P.; Dalton, M.; Fedorova, Y.; Field, C.; Hast, C.; Huang, M. A.; Hüntemeyer, P.; Hwang, W. Y. P.; Iverson, R.; Jones, B. F.; Jui, C.; Lin, Guey-Lin; Loh, E. C.; Manago, Naohiro; Martens, K.; Matthews, J. N.; Maestas, M. M.; Ng, J.; Odian, A.; Reil, K.; Rodriguez, D.; Smith, J. D.; Sokolsky, P.; Springer, R. W.; Thomas, J. R.; Thomas, S. B.; Thomson, G. B.; Walz, D.; Zech, A.

doi:10.1016/j.nima.2008.08.054

Cited by 4 publications

(2 citation statements)

References 14 publications

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“…For reasons of keeping a historically consistent energy scale, the HiRes and TA groups have used the original Kakimoto et al overall yield measurement [65] while a subset of Auger collaborators has launched a series of special experiments to measure the fluorescence yield more precisely with AIRFLY [67,154]. The HiRes group also performed a series of measurements using an electron beam at SLAC (FLASH [155][156][157]) but only the relative spectral line strength measurement has so far been incorporated in the TA analysis. The TA experiment also includes a 40 MeV electron linac whose vertical beam is seen in the field of view of one of the fluorescence detectors.…”

Section: Energymentioning

confidence: 99%

Past, Present and Future of UHECR Observations

Dawson

Fukushima

Sokolsky

2017

Preprint

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Great advances have been made in the study of ultra-high energy cosmic rays (UHECR) in the past two decades. These include the discovery of the spectral cut-off near 5 × 10 19 eV and complex structure at lower energies, as well as increasingly precise information about the composition of cosmic rays as a function of energy. Important improvements in techniques, including extensive surface detector arrays and high resolution air fluorescence detectors, have been instrumental in facilitating this progress. We discuss the status of the field, including the open questions about the nature of spectral structure, systematic issues related to our understanding of composition, and emerging evidence for anisotropy at the highest energies. We review prospects for upgraded and future observatories including Telescope Array, Pierre Auger and JEM-EUSO and other space-based proposals, and discuss promising new technologies based on radio emission from extensive air showers produced by UHECR.

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Section: Energymentioning

confidence: 99%

Past, Present and Future of UHECR Observations

Dawson

Fukushima

Sokolsky

2017

Preprint

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“…These groups have been discussing their techniques and data in a series of Air Fluorescence Workshops (AFW) commenced in Utah, 2002 [9]. Main results are contributed by the following alphabetic list of collaborations and groups led by their principal investigators: AIRFLY [10,11,12,13,14,15], Airlight [16,17], Arqueros/UCM [18,19,20,21,22], FLASH [23,24,25,26], Fraga/LIP [27,28], Keilhauer/KIT [29,30,31], Lefeuvre/APC [32], MACFLY [33], Nagano/Sakaki [34,35,36], and Ulrich/TUM [37,38,39,40]. At the up to now last Air Fluorescence Workshop in Karlsruhe, 2011, it was decided to develop a common fluorescence description for application at air shower reconstructions [9].…”

Section: Introductionmentioning

confidence: 99%

Nitrogen fluorescence in air for observing extensive air showers

Keilhauer

Bohã̌cov́a

Fraga

et al. 2013

EPJ Web of Conferences

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Abstract. Extensive air showers initiate the fluorescence emissions from nitrogen molecules in air. The UVlight is emitted isotropically and can be used for observing the longitudinal development of extensive air showers in the atmosphere over tenth of kilometers. This measurement technique is well-established since it is exploited for many decades by several cosmic ray experiments. However, a fundamental aspect of the air shower analyses is the description of the fluorescence emission in dependence on varying atmospheric conditions. Different fluorescence yields affect directly the energy scaling of air shower reconstruction. In order to explore the various details of the nitrogen fluorescence emission in air, a few experimental groups have been performing dedicated measurements over the last decade. Most of the measurements are now finished. These experimental groups have been discussing their techniques and results in a series of Air Fluorescence Workshops commenced in 2002.At the 8 th Air Fluorescence Workshop 2011, it was suggested to develop a common way of describing the nitrogen fluorescence for application to air shower observations. Here, first analyses for a common treatment of the major dependences of the emission procedure are presented. Aspects like the contributions at different wavelengths, the dependence on pressure as it is decreasing with increasing altitude in the atmosphere, the temperature dependence, in particular that of the collisional cross sections between molecules involved, and the collisional de-excitation by water vapor are discussed.

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