The age pattern across spiral arms is one of the key observational features utilised to study the dynamic nature of the Galaxy’s spiral structure. With the most updated samples of high-mass star formation region (HMSFR) masers, O stars and open clusters, we investigated their distributions and kinematic properties in the vicinity of the Sun. We found that the Sagittarius-Carina Arm traced by HMSFRs, O stars (≲ 10 Myr) and young open clusters (<30 Myr) seem to deviate gradually towards the Galactic Anticenter (GAC) direction. The Local Arm traced by HMSFRs, O stars, young clusters and also medium-young clusters (30–100 Myr) are inclined to gradually deviate toward the Galactic Center (GC) direction. The properties for the Local Arm are supported by a simplified simulation of cluster motions in the Galaxy. Indications of systematic motions in the circular and radial velocities are noticed for the old open clusters (>200 Myr). These results are consistent with the idea that star formation can be triggered by spiral shocks of density waves, and indicate that the corotation radius of the Galaxy is located between the Sagittarius-Carina Arm and the Local Arm, close to the Solar circle.

跨旋臂的年龄格局是用来研究银河旋涡结构动态性质的关键观测特征之一。利用最新的高质量恒星形成区（HMSFR）masers，O恒星和疏散星团的样本，我们研究了它们在太阳附近的分布和运动学性质。我们发现，由HMSFR，O星（≲10 Myr）和年轻的疏散星团（<30 Myr）追踪的人马座臂似乎朝银河系反中心（GAC）方向逐渐偏离。由HMSFR，O星，年轻星团以及中年轻星团（30–100 Myr）追踪到的局部臂倾向于向银河系中心（GC）方向逐渐偏离。简化了银河系中星团运动的模拟，为“本地手臂”的属性提供了支持。对于旧的开放星团（> 200 Myr），注意到在圆周速度和径向速度上系统运动的迹象。这些结果与以下想法相一致：恒星形成可以由密度波的螺旋激波触发，并表明银河系的正转半径位于人马座-船腹臂和本地臂之间，靠近太阳圆。