Newest CCD Positions for Saturn and Its Major Satellites
Based on CCD images taken with the 1 m telescope at the Yunnan Obser vatory during the years 2002-2006, more than two thousand precise positions of Saturn and its major satellites were derived. We improved image-processing techniques for the pixel positional measurement for Satums rings and its major satellites. When the four bright satellites S3-S6 of Saturn are used to calibrate the CCD field of view by com paring their pixel positions with their theoretical ones from the theory TASS1.7, the observational positions of all major satellites when measured with respect to Rhea are found to have usually a good agreement with their theoretical ones except for Mimas. However, this systematic error of Mimas becomes much smaller when the recent JPL ephemeris of Mimas is replaced. Our rms (root-meansquares) errors in each coordi nate are about 40 mas for Saturn and its bright satellites S3-S6, and 50 and 90 mas for Enceladus and Mimas, respectively.
planet and satellite astrometry rings technique image-processing
Q. Y. Peng Q. F. Zhang N. Wang
Department of Computer Science, Jinan University, Guangzhou 510632, China Joint Laboratory of Optica Department of Computer Science, college of Zengcheng, South China Normal University, Guangzhou 51136
国际会议
The 10th Asian-Pacific Regional International Astronomical Union Meeting(第十届亚洲及太平洋地区天文学大会 APRIM)
昆明
英文
390-392
2008-08-03（万方平台首次上网日期，不代表论文的发表时间）