Hostname: page-component-586b7cd67f-dlnhk Total loading time: 0 Render date: 2024-12-01T10:33:51.020Z Has data issue: false hasContentIssue false
  • English
  • Français

A Note on the Astrometric Precision of Minor Planet Observations

Published online by Cambridge University Press:  12 April 2016

D. Pascu
D. Pascu*
Affiliation:
U. S. Naval Observatory Washington, DC 20392-5100USA.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

For years, interest in precise positions of minor planets has centered on tying the dynamical reference frame with the stellar frame and determining catalog zone errors. Photographic methods are generally used in obtaining observed spherical equatorial coordinates (R.A., Dec.) or crossing-point observations. Estimates of the external precision of the equatorial coordinates are overly pessimistic, while those for crossing-point observations, too optimistic.

It is estimated that equatorial positions for the brighter (m < 11) minor planets can be determined with an external precision not worse than +/−0.2 arcsec (m.e.), and perhaps as low as +/−0.1 arcsec (m.e.), depending on the reference catalog zonal errors.

Intersatellite observations are a type of crossing-point observation in which the images of two different objects appear in the same exposure. This is the most precise type of crossing-point observation and gives an estimate for the lower limit to the external precision of this observation type. Recent studies of satellite observations indicate that this lower limit is in the +/−0.05 to +/−0.08 arcsec (m.e.) range.

Type
Part 2. Poster Papers
Information
International Astronomical Union Colloquium , Volume 127: Reference Systems , 1991 , pp. 327 - 330
Copyright
Copyright © United States Naval Observatory 1991

References

De Vegt, Chr.: 1988, in Mapping the Sky, IAU Symposium No. 133, eds. Debarbat, S., Eddy, J.A., Eichhorn, H.K. and Upgren, A. R., Reidel, Dordrecht, p. 211.Google Scholar
Douglass, G.G. and Harrington, R.S.: 1990, Astron. J. 100, 1712.Google Scholar
Hemenway, P.: 1980, Cel. Mech. 22, 89.Google Scholar
Orelskaya, V.I.: 1974, in Asteroids, Comets and Meteoric Matter, IAU Colloquium No. 22, eds. Cristescu, C., Klepczynski, W.J. and Milet, B., Editura Academiei, Bucharest, p. 39.Google Scholar
Pascu, D. and Schmidt, R.E.: 1990, Astron. J. 99, 1974.Google Scholar
Pierce, D.A.: 1978, Astron. Pap. American Ephem. XXII, pt. III, p.207.Google Scholar
Taylor, D.B.: 1985, 1986, private communication.Google Scholar
Taylor, D.B. and Shen, K.X.: 1988, Astron. Astrophys. 200, 269.Google Scholar
Whipple, A.L., Duncombe, R.L. and Hemenway, P.D.: 1988, in The Earth’s Rotation and Reference Frames for Geodesy and Geodynamics, IAU Symposium No. 128, eds. Babcock, A. K. and Wilkins, G. A., Reidel, Dordrecht, p. 55.Google Scholar