2018ApJ...866...20D

To probe the star formation process, we present a thorough multiwavelength investigation of several H II regions located toward l = 24.°8, b = 0.°1. A system of at least five H II regions, including the mid-infrared bubble N36 (hereafter system N36; extension ∼35 pc), is observationally investigated and is located at a distance of 6.0 kpc. With this distance, the system N36 is found to be situated at the interface of the Galactic bar and the Norma Galactic arm in our Galaxy, where one may expect the collisions of molecular clouds due to the bar potential. Each H II region (dynamical age ∼0.4-1.3 Myr) in the system is powered by an O-type star. The system contains 27 ATLASGAL dust clumps at 870 µm. Several clumps are massive (>10³ M_☉) and have high bolometric luminosity (>10³ L_☉). Using the GRS ¹³CO line data, in the direction of the system N36, two velocity components are found around 109 and 113 km s^–1 and are linked in the velocity space. The morphological analysis of ¹³CO favors the presence of interacting molecular clouds in the system. Four H II regions and two 6.7 GHz masers are spatially observed at the common areas of the two clouds. The analysis of the Spitzer photometric data also traces the noticeable star formation activity in the system. Considering the observational outcomes, the formation of O-type stars (including ongoing star formation) in the system appears to be triggered by the collisions of molecular clouds at the bar-arm interface.