A Kinematical Calibration of the Galactocentric Distance
A Kinematical Calibration of the Galactocentric Distance
复制标题
DOI：
10.1088/1009-9271/7/1/09
复制
发表时间：
2007-02
期刊：
影响因子：
--
通讯作者：
M. Shen;Zi Zhu
中科院分区：
文献类型：
--
作者：
M. Shen;Zi Zhu
我们提出了用纯运动学模型确定星系中心距离的新方法。银河系薄盘的两个组成亚群，O-B5恒星和银河系疏散星团，被选择用于我们的分析。根据大约1200颗O-B5恒星的运动数据，我们得到了R0= 8.25±0.79 kpc，而270个银河系疏散星团的R0=7.95±0.62kpc。考虑到个别研究者用不同方法给出的R0的离散性，我们目前的确定结果与里德提出的最佳值非常吻合。
We present a new determination of the Galactocentric distance by a pure kinemat- ical model. Two subgroups of components from the Galactic thin disk, the O-B5 stars and the Galactic open clusters, were selected for our analysis. On the basis of kinematical data of around 1200 O-B5 stars, we obtained an estimated value of R 0=8.25±0.79 kpc, while a similar evaluationfrom 270 Galactic open clusters gives R0=7.95±0.62kpc. Considering the scatter of R0 given by individual investigators with different methods, our present determi- nations agree well with the best value proposed by Reid.