A Dynamical Model for the Globular Cluster G1
A Dynamical Model for the Globular Cluster G1
复制标题
球状星团G1的动力学模型
DOI：
10.1086/375802
复制
发表时间：
2003
期刊：
影响因子：
--
通讯作者：
Simon Portegies Zwart
中科院分区：
文献类型：
--
作者：
H. Baumgardt;Junichiro Makino;P. Hut;S. McMillan;Simon Portegies Zwart
我们给出了用哈勃空间望远镜广域行星相机2和空间望远镜成像光谱仪获得的M31中G1的运动结构的观测数据与用专用计算机GRAPE-6进行的动力学模拟结果的比较。对于从单星系团King模型初始条件开始的模型，我们获得了很好的拟合，当我们以动态构建的两个星系团的合并产品开始模拟时，我们的拟合更好。在后一种情况下，我们的模拟结果与观测到的光度、速度色散、旋转和椭圆度的轮廓非常一致。得到了质光比M/L=4.0±0.4，团簇总质量M=(8±1)×10~6M☉。鉴于我们的动力学模型可以很好地符合所有可用的观测数据，似乎没有必要援引在G1中心存在中等质量黑洞的说法。
We present a comparison between the observational data on the kinematical structure of G1 in M31, obtained with the Hubble Space Telescope Wide Field Planetary Camera 2 and Space Telescope Imaging Spectrograph instruments, and the results of dynamical simulations carried out using the special purpose computer GRAPE-6. We have obtained good fits for models starting from single-cluster King model initial conditions and even better fits when starting our simulations with a dynamically constructed merger product of two star clusters. In the latter case, the results from our simulations are in excellent agreement with the observed profiles of luminosity, velocity dispersion, rotation, and ellipticity. We obtain a mass-to-light ratio of M/L = 4.0 ± 0.4 and a total cluster mass of M = (8 ± 1) × 106 M☉. Given that our dynamical model can fit all available observational data very well, there seems to be no need to invoke the presence of an intermediate-mass black hole in the center of G1.