Very High Energy Gamma Ray Astronomy at White Cliffs Solar Power Station

Clay, R. W.; Elton, Stephen D.; Gregory, A. G.; Patterson, Joseph; Protheroe, R. J.

doi:10.1017/s1323358000027028

Cited by 6 publications

(3 citation statements)

References 6 publications

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“…There are currently nine VHE 7-ray telescopes in operation, only two of these being located in the Southern Hemisphere (the telescope operated by the Adelaide group at White Cliffs, N.S.W., is described in this volume by Clay et al 1986). The properties of these telescopes are summarized in Table 1.…”

Section: Vhe 7-ray Observationsmentioning

confidence: 99%

Gamma-Ray Astronomy at the Highest Energies

Protheroe

1986

Publ. Astron. Soc. Aust.

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In 1983 ultra high energy γ-rays were detected from Cygnus X-3. This was of particular interest since it is the first identifiable source of cosmic rays. Since then, there has been an explosion of interest in the field with more than twenty air shower arrays planned or being used to search for γ-rays at energies above 1014 eV. Observational techniques for both very high energy and ultra high energy γ-ray astronomy are described and existing and proposed experiments reviewed with particular reference to their geographical locations. The results obtained so far are summarised together with some of the models proposed to explain them.

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Section: Vhe 7-ray Observationsmentioning

confidence: 99%

Gamma-Ray Astronomy at the Highest Energies

Protheroe

1986

Publ. Astron. Soc. Aust.

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“…Techniques based on the shape of the lateral distribution and fast timing of the Cerenkov light pool to delineate source direction, have been studied [3,4]. The successful imaging technique is most sensitive at small zenith angles.…”

Section: Introductionmentioning

confidence: 99%

Pulse shape selection in very high energy gamma-ray astronomy

Roberts¹,

Edwards²,

Patterson³

et al. 1998

J. Phys. G: Nucl. Part. Phys.

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Very high energy gamma-ray astronomers using the atmospheric Čerenkov technique must contend with a large background of light pulses due to cosmic ray-initiated cascades. Significant advances have been made in developing techniques to reduce this background: the imaging technique can have a figure of merit, q, in excess of 6 near the zenith. However, q decreases as the zenith angle increases. In this paper we describe a new technique based on the temporal Čerenkov pulse shape and show that the use of rise time and FWHM cuts are effective discriminators at all zenith angles. For flat-spectrum sources at large zenith angles q ∼ 2.5. Measured parameter distributions are compared with simulations and the methods of making the cuts are discussed. A sensitivity to cosmic-ray composition is also suggested.

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“…The University of Adelaide, building upon experience gained with earlier experiments at Buckland Park (Abies et al 1969) and White Cliffs (Clay et al 1986), has operated since 1988 a VHE gamma-ray telescope 15 km north of Woomera. The site (31°6'S, 136°47'E, 160 m a.s.l.)…”

Section: The Bicentennial Gamma-ray Telescopementioning

confidence: 99%

The CANGAROO Project: Very High Energy Gamma-ray Astronomy at Woomera

Edwards

Gregory

Patterson

et al. 1992

Publ. Astron. Soc. Aust.

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In this paper the Very High Energy (VHE) gamma-ray astronomy program at the University of Adelaide is described. VHE gamma rays with energies above ~5 × 1011eV are observed using the atmospheric Cerenkov technique. Results from the first three years observations at Woomera and the current upgrading of the telecope are described. The CANGAROO project, a collaboration between the University of Adelaide and a number of Japanese institutions, is also introduced.

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Very High Energy Gamma Ray Astronomy at White Cliffs Solar Power Station

Cited by 6 publications

References 6 publications

Gamma-Ray Astronomy at the Highest Energies

Gamma-Ray Astronomy at the Highest Energies

Pulse shape selection in very high energy gamma-ray astronomy

The CANGAROO Project: Very High Energy Gamma-ray Astronomy at Woomera

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