论文标题
一种以银河系来定义螺旋臂宽度的新的多跟踪方法
A New Multi-Tracer Approach to Defining the Spiral arm width in the Milky Way
论文作者
论文摘要
我们分析了银河半径的最新观察结果，该观察结果是银河半径的函数，并将这种关系与密度波理论的预测进行了比较。我们使用以下方法：在每个螺旋臂中，我们集中于密度波的冲击前方附近的星形区域（无线电元）之间的分离（或偏移），以及密度最小的衰老恒星区域（漫游者CO气）在密度波的潜在最小值附近；我们将这两个示踪剂之间的分离作为手臂宽度。 新结果：我们在250 +/- 50 pc附近发现了一个典型的分离（Maser到分散CO气体），并且每千台下的银河半径约为25 +/- 5 pc，这种分离的增加。我们注意到，正如预期的那样，这种分离要比尘埃道和老化恒星区域之间的分离要小一些。总体而言，这些结果支持密度波的基础。
We analyze recent observations of the spiral arm width in the Milky Way, as a function of the galactic radius, and we compare this relation with the prediction from the density wave theory. We use the following method: in each spiral arm, we concentrate on the separation (or offset) between the starforming region (radio masers) near the shock front of a density wave, and the aged star region (diffuse CO gas) near the potential minimum of a density wave; we take this separation between these two tracers as the arm width. New results: we find a typical separation (maser to diffuse CO gas) near 250 +/- 50 pc, and an increase of this separation with galactic radius of about 25 +/- 5 pc per kpc. We note that, as expected, this separation is somewhat smaller than that found earlier between the dust lane and the aged star region. Overall, these results supports the basics of a density wave.
