Hostname: page-component-78c5997874-xbtfd Total loading time: 0 Render date: 2024-11-16T09:21:21.918Z Has data issue: false hasContentIssue false

Asteroid Discovery Efficiencies for Telescope Systems at Siding Spring

Published online by Cambridge University Press:  25 April 2016

Duncan Steel*
Affiliation:
Anglo-Australian Observatory, Private Bag, Coonabarabran, NSW 2357, Australia; and Department of Physics and Mathematical Physics, University of Adelaide, Adelaide, SA [email protected], or, [email protected]

Abstract

Relative efficiencies for the discovery of Earth-crossing asteroids (ECAs) are modelled for various telescopes at Siding Spring. It is found that the narrow-field instruments—the Anglo-Australian Telescope and the 40 in and 2·3m reflectors—are not competitive in this regard for present CCD imaging systems. The UK Schmidt Telescope (UKST), if used to take short-exposure stereo pairs of photographs, would be an effective search tool, outperforming all current systems apart from the Ground-based Electro-Optical Deep Space Surveillance (GEODSS) systems now being implemented by the US Air Force for ECA searches. If a CCD mosaic were fitted to the UKST, its performance would far exceed that of any other device at Siding Spring, and it would produce ECA discoveries at a rate around 3–4 times as high as GEODSS, but at considerable expense. The most sophisticated search instrument currently in use is the University of Arizona’s Spacewatch telescope; a notable result found here is that even with its present CCD, the Automated Patrol Telescope (APT) of the University of New South Wales would be able to match or outperform Spacewatch for all ECA sizes, including ~10m objects, should this modelling be a reasonable representation of its real performance. In terms of cost-effectiveness and telescope availability, the conclusion arrived at herein is that the APT, equipped with small-pixel but large-format CCD chips of high quantum efficiency, would be an extremely effective ECA search instrument: if operated with 12 μm pixel chips covering a 4° × 4° field it might produce ECA discoveries at a rate well in excess of the combined rate for all current search programs.

Type
Solar and Solar System
Copyright
Copyright © Astronomical Society of Australia 1995

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Carter, B. D., Ashley, M.C.B., Sun, Y. S., & Storey, J. W. V., 1992, PASA, 10, 74 Google Scholar
Chapman, C. R., & Morrison, D., 1994, Nature, 367, 33 CrossRefGoogle Scholar
Gehrels, T., 1991, Space Sci. Rev., 58, 347 Google Scholar
Gehreis, T. (ed.) 1994, Hazards due to Comets and Asteroids (Tucson: Univ. of Arizona Press)Google Scholar
Harris, A. W., 1994, in Seventy-Five Years of Hirayama Asteroid Families, ed. Kozai, Y., Binzel, R. P. & Hirayama, T., Astron. Soc. Pacific Conf. Series, 63, 203 Google Scholar
Lewis, J. S., Matthews, M. S., & Guerrieri, M. L. (eds), 1993, Resources of Near-Earth Space (Tucson: Univ. of Arizona Press)Google Scholar
Marsden, B. G., & Steel, D. I., 1994, in Hazards due to Comets and Asteroids, ed. Gehreis, T. (Tucson: Univ. of Arizona Press), 221 Google Scholar
Morrison, D., 1992, The Spaceguard Survey: Report of the NASA International Near-Earth-Object Detection Workshop (Pasadena: Jet Propulsion Laboratory)Google Scholar
Rabinowitz, D. L., 1991, AJ, 101, 1518 Google Scholar
Rabinowitz, D. L., 1994, Icarus, 111, 364 Google Scholar
Rabinowitz, D., Bowell, E., Shoemaker, E., & Muinonen, K., 1994, in Hazards due to Comets and Asteroids, ed. Gehrels, T. (Tucson: Univ. of Arizona Press), 285 Google Scholar
Steel, D., 1992, in Proceedings of the Near-Earth Object Interception Workshop, ed. Canavan, G. H. Solem, J. C. & Rather, J. D. G. (Los Alamos: Los Alamos National Laboratory), LA-12476-C, 62 Google Scholar
Steel, D. I., 1995, MNRAS, 273, 1091 Google Scholar
Steel, D., & McNaught, R. H. 1991, Aust. J. Astron., 4, 42 Google Scholar