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6 Conclusion

The CCD observing campaigns we made at the Sheshan Station during 1994-1996 years are successful. The excellent 1.56m astrometric reflector provided by the observatory together with the good seeing permitted us to obtain the better quality results than photographic observation of Saturn's satellites. Especially, we have now obtained some valuable measurements for the faint satellites, which are usable for improving their theories. Our reduction also shows that the method we used to define the reference system for solving the calibration parameters was adequate for our purpose. From this we have now found in our published data (1996) an inaccurate scale which leads to the overlarge residuals, in particular for $\triangle S$. We will continue to develop such research for observation of the Saturnian satellite system.

Acknowledgements

Authors wish to thank Prof. B.C. Qian and his staff at the Sheshan Station for their kind assistance. We are also grateful to Dr. Vienne for providing us his new version TASS1.7. We would like to thank Dr. Gerard Dourneau for his helpful comments of this paper. Especial emphasis must be placed on that this work was carried out with financial support from National Natural Science Foundation of China (NSFC) and Astronomy Research Council.


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