Determination of kinematic distances of <i>WISE</i> and SMGPS H  <scp>ii</scp> regions in the Galactic plane using SEDIGISM cloud association

Abstract

ABSTRACT 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, 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 MeerKAT Galactic Plane Survey with molecular clouds from the Structure, Excitation and Dynamics of the Inner Galactic Interstellar Medium (SEDIGISM) $^{13}$CO (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 3.46 km s$^{-1}$. 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.