Abstract

A three-component Stäckel model of the Galaxy, including the bulge, disk, and halo, is constructed. Parameter estimates of the potential are obtained as a result of fitting the model rotation curve to azimuthal velocities found from data on trigonometric parallaxes and spatial velocities of masers. The fitting method takes into account the measurement and natural dispersions of azimuthal velocities and uses an algorithm for excluding objects with excessive residuals. In order to obtain more uniform samples, the objects were divided into two groups: masers associated with high-mass star forming regions and masers of other types. A significant kinematic inhomogeneity of these groups was identified and taken into account: the azimuthal velocity dispersion is \({{\sigma }_{{0,1}}} = 4.3 \pm 0.4\) km s^–1 in the first group and \({{\sigma }_{{0,2}}} = 15.2 \pm 1.3\) km s^–1 in the second. After constructing the model of the Galactic-plane potential, it was generalized to the entire space under the assumption of the existence of a third quadratic integral of motion. When reconstructing the Galactic rotation curve in detail, the used algorithm gives an analytical expression for the Stäckel potential, which significantly simplifies the task of constructing the Galaxy's phase density model in the Stäckel approximation. In order to make the Stäckel model more realistic, one needs to develop methods of direct account of data on the vertical distribution of density in the Galaxy.

中文翻译：

---

基于Maser数据旋转曲线的星系三分量Stäckel模型

摘要

构建了星系的三分量 Stäckel 模型，包括凸起、圆盘和光晕。作为将模型旋转曲线拟合到从三角视差和脉泽空间速度数据中找到的方位速度的结果，获得了势能的参数估计。拟合方法考虑了方位角速度的测量和自然分散，并使用一种算法来排除具有过多残差的对象。为了获得更均匀的样本，天体被分为两组：与大质量恒星形成区相关的脉泽和其他类型的脉泽。确定并考虑了这些组的显着运动不均匀性：方位角速度色散为\({{\sigma }_{{0,1}}} = 4.3 \pm 0.4\) km s^–1在第一组和\({{\sigma }_{{0,2}}} = 15.2 \pm 1.3\) km s ^–1在第二组。建立银面势模型后，假设存在三次运动二次积分，将其推广到整个空间。在详细重建银河自转曲线时，所使用的算法给出了 Stäckel 势的解析表达式，这大大简化了在 Stäckel 近似中构建银河系相密度模型的任务。为了使 Stäckel 模型更加真实，人们需要开发直接解释银河系密度垂直分布数据的方法。