AI 中文总结
该研究提出通过云关联确定银道面WISE和SMGPS H II区运动学距离的方法，将其与SEDIGISM分子云关联，通过空间和速度建立联系，验证了方法有效性，解决部分速度模糊问题，提供了距离目录并建立研究框架。
AI 中文摘要
研究和理解银河系结构与大质量恒星形成的基本要求之一是准确测定H II区的距离。然而，大多数距离测定受运动学距离模糊性、稀疏视差测量以及大量缺乏速度和距离测量的射电连续谱源的阻碍。我们提出一种通过云关联确定运动学距离的方法，将广域红外巡天探测器（WISE）目录和南非射电天文台（SARAO）MeerKAT银道面巡天（SMGPS）中的H II区与来自银河系内星际介质的结构、激发和动力学（SEDIGISM）13CO（2-1）巡天的分子云关联起来。通过空间重叠和速度一致性建立关联，然后将分子云的速度和距离赋予相关的H II区。该方法得出741个采用基于CO的系统速度的H II区，其中640个根据SEDIGISM距离可靠性标准有可靠的运动学距离。我们用329个具有独立射电复合线（RRL）速度的H II区验证了该方法，发现中位数绝对速度差为3.46km/s，一致性良好。我们的分析解决了40个有多个WISE RRL速度测量的H II区的速度模糊问题。与未关联的云相比，关联的分子云质量、气体表面密度、线宽、恒星形成效率和致密气体分数显著更高，维里参数略低。这项工作提供了一个大量、均匀推导的H II区距离目录，并建立了一个进一步研究大质量恒星形成和银河系结构的框架。
英文摘要
One of the fundamental requirements for studying and understanding Galactic structure and massive star formation is accurate distances to H II regions. However, most distance assignments are hampered by kinematic distance ambiguity (KDA), sparse parallax measurements, and the large number of radio continuum sources lacking velocity and distance measurements. We present a kinematic distance determination method via cloud association, linking H II regions from the Wide-field Infrared Survey Explorer (WISE) catalogue and the South African Radio Astronomy Observatory (SARAO) MeerKAT Galactic Plane Survey (SMGPS) with molecular clouds from the Structure, Excitation and Dynamics of the Inner Galactic Interstellar Medium (SEDIGISM) 13CO (2-1) survey. The associations are established through spatial overlap and velocity coherence, and the molecular cloud velocity and distance are then assigned to the associated H II region. The method yields 741 H II regions with adopted CO-based systemic velocities, of which 640 have reliable kinematic distances based on the SEDIGISM distance reliability criteria. We validate the method using 329 H II regions with independent radio recombination line (RRL) velocities, finding excellent agreement with a median absolute velocity difference of 3.46km/s. Our analysis resolves ambiguous velocities for 40 H II regions with multiple WISE RRL velocity measurements. Compared to the unassociated clouds, the associated molecular clouds exhibit significantly higher masses, gas surface densities, linewidths, star formation efficiencies and dense gas fractions, and slightly lower virial parameters. This work provides a large, homogeneously-derived catalogue of H II region distances and establishes a framework for further studying massive star formation and Galactic structure in general.
