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Two-point Angular Autocorrelation Function and the Origin of the Highest-energy Cosmic Rays

Published online by Cambridge University Press:  05 March 2013

R. W. Clay ,
B. R. Dawson ,
L. Kewley  and
M. Johnston-Hollitt
R. W. Clay
Affiliation:
Department of Physics and Mathematical Physics, University of Adelaide, SA 5005, Australia; [email protected]
B. R. Dawson
Affiliation:
Department of Physics and Mathematical Physics, University of Adelaide, SA 5005, Australia
L. Kewley
Affiliation:
Research School of Astronomy and Astrophysics, Australian National University, Weston Creek PO, Weston, ACT 2611, Australia; [email protected]
M. Johnston-Hollitt
Affiliation:
Department of Physics and Mathematical Physics, University of Adelaide, SA 5005, Australia
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Abstract

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Construction of the Pierre Auger Observatory for the study of the highest-energy cosmic rays is about to begin. Prior to the availability of data from that experiment, decisions should be made on techniques for the analysis of the directional properties of those data. We examine here one possible analysis tool, the two-point angular autocorrelation function. As a concrete example, data from the SUGAR array are examined in this way. Possible clustering of the data is observed, and the identification of such clustering with candidate astronomical objects in a purpose-developed catalogue is investigated.

Keywords

methods: data analysiscosmic raysgalaxies: intergalactic medium
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 17 , Issue 3 , 2000 , pp. 207 - 211
Copyright
Copyright © Astronomical Society of Australia 2000

References

Allen, W. H., et al. 1993, Astroparticle Physics, 1, 269Google Scholar
Clay, R. W., Dawson, B. R., & Meyhandan, R. 1994, Astroparticle Physics, 2, 347 Google Scholar
Clay, R. W., et al. 1998, Astroparticle Physics, 9, 221 Google Scholar
Clay, R. W., et al. 2000, Astroparticle Physics, 12, 249 CrossRefGoogle Scholar
Hartle, J. B., Thorne, K. S., & Price, R. H., 1986, in Black Holes: The Membrane Paradigm, ed. K. S. Thorne, R. H Price & D. A. McDonald (New Haven: Yale University Press), p. 160 Google Scholar
Hayashida, N., et al. 1999, Astroparticle Physics, 10, 303 Google Scholar
Hillas, A. M. 1984, ARA&A, 22, 425 Google Scholar
Ikebe, Y., et al. 1997, ApJ, 481, 6601 Google Scholar
Jackson, C. A. 1999, PASA, 16, 124 Google Scholar
Lampard, R., Clay, R. W., & Dawson, B. R. 1997a, PASA, 14, 258 Google Scholar
Lampard, R., Clay, R. W., & Dawson, B. R. 1997b, Astroparticle Physics, 7, 213 Google Scholar
Muecke, A., et al. 1999, PASA, 16, 160 CrossRefGoogle Scholar
Peebles, P. J. E. 1980, in The Large Scale Structure of the Universe (Princeton: Princeton University Press), p. 174 Google Scholar
Robertson, J. G. 1973, Aust. J. Phys., 26, 403 CrossRefGoogle Scholar
Winn, M. M., et al. 1986, J. Phys. G: Nucl. Phys., 12, 653 CrossRefGoogle Scholar