EDP Sciences
Free access
Volume 391, Number 2, August IV 2002
Page(s) 775 - 779
Section Celestial mechanics and astrometry
DOI http://dx.doi.org/10.1051/0004-6361:20020872

A&A 391, 775-779 (2002)
DOI: 10.1051/0004-6361:20020872

Astrometry of five major Uranian satellites in 1995-1997

K. X. Shen1, 2, 3, R. C. Qiao1, 3, D. Harper4, K. G. Hadjifotinou5 and J. R. Liu1, 3

1  Shaanxi Astronomical Observatory, The Chinese Academy of Science, Lintong, Shaanxi 710600, PR China
2  Chinese National Astronomical Research Center
3  United Laboratory for Optical Astrometry, The Chinese Academy of Science, PR China
4  Wellcome Trust Sanger Institute, Wellcome Trust Genome Campus, Hinxton, Cambridge CB10 1SA, UK
5  Department of Mathematics, Faculty of Science, Aristotle University of Thessaloniki, 54006 Thessaloniki, Greece

(Received 19 November 2001 / Accepted 6 June 2002)

At the oppositions of 1995-1997, a total of 122 CCD frames were taken on the 1.56 m astrometric telescope at the Sheshan station, yielding 864 positions of the major Uranian satellites. The calibration of the images was carried out using a least-squares iterative program by fitting to the well-known orbits of the brighter moons of Uranus, based on the modern theory GUST86 and an ephemeris produced by numerical integration. The residuals lay between $0\farcs03$ and $0\farcs05$ for each of the inter-satellite positions, except for the innermost and faintest satellite Miranda, whose residuals exceeded $0\farcs08$ due to the proximity of Uranus. No significant systematic errors were found when using satellites themselves for determining calibration parameters. The largest residual in the comparison between GUST86 and the numerical integration was about $0\farcs01$.

Key words: planets and satellites: general

Offprint request: K. X. Shen, shenkx@ms.sxso.ac.cn

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