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Shower Detection Methods and Basic Event Reconstruction

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Extensive Air Showers

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Overview

This chapter contains an outline of the different air shower detection methods, many of which are discussed in detail in dedicated chapters later on. Detection techniques that had been explored only briefly in the past or are presently in an exploratory phase, such as radar ranging and acoustic detection, respectively, are not treated in separate chapters but are discussed extensively here. Directly and indirectly accessible shower parameters are introduced and briefly described, followed by the elementary concepts of shower reconstruction and a brief overview of the response of common particle detectors to shower particles, including transition effects. Indirectly accessible parameters are discussed in Chap. 10.

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Notes

  1. 1.

    In some applications only sectors of a hemispherical detector geometry are being used that cover a restricted solid angle of the sky, such as is the case at the Auger Observatory (Blümer

  2. 2.

    The layout of a selection of air shower particle detector arrays of the past and present are displayed in Sect. A.1.

  3. 3.

    Note that trigger conditions may be set such that event selection can be influenced in many ways to meet special requirements.

  4. 4.

    Mainly low energy muons and electrons, but also photons via conversion processes in the water that produce positron–negatron pairs, Compton scattered and knock-on electrons are being recorded.

  5. 5.

    Relativistic muons lose about 2 MeV g−1 cm2.

  6. 6.

    Using special ultraviolet sensitive photomultiplier tubes and/or appropriate filters in front of the photomultipliers permit to operate an optical atmospheric Cherenkov array at certain times during the presence of the moon.

  7. 7.

    Note that showers whose axis is directed towards a fluorescence detector or its immediate vicinity are usually excluded from analysis because the intense Cherenkov beam obscures the fluorescence signal.

  8. 8.

    The Fly’s Eye detector had in fact been operated jointly at times with the CASA-MIA, BLANCA and DICE arrays at Dugway (Utah) (Bird et al., 1995; Cassidy et al., 1997; Swordy and Kieda, 2000).

  9. 9.

    At present geo-synchrotron radiation is believed to be the chief contributor.

  10. 10.

    Micro meteorites having masses as small as \(\sim 1\,\upmu\)g and diameters \(\simeq 0.1\) mm may cause ionization line densities in the atmosphere on the order of \(\sim 10^{13}\) electrons m−1 which are detectable by RADAR (Gorham, 2001).

  11. 11.

    According to Askar’yan (1979) the acoustic signal estimated by Bowen in this chapter is grossly overestimated by a factor of 107–108.

  12. 12.

    Tracking detectors, though only seldom used, reveal directly the direction of propagation of the shower particles. The claimed angular accuracy of this method is \(\sim 0.3^{\circ}\).

  13. 13.

    This is also valid for large showers where the particle disk manifests a curved surface.

  14. 14.

    The altitude is relevant because of the energy of the particles.

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  1. University of Bern Physikalisches Institut, Sidlerstr. 5, 3012, Bern, Switzerland

    Prof. Dr. Peter K.F. Grieder

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Grieder, P.K. (2010). Shower Detection Methods and Basic Event Reconstruction. In: Extensive Air Showers. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-76941-5_2

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