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To probe the star formation (SF) process, we present a thoroughmulti-wavelength investigation of several H II regions located toward l = 24.8deg, b = 0.1 deg. A system of at least five H II regions including themid-infrared bubble N36 (hereafter "system N36"; extension ~35 pc) isobservationally investigated, and is located at a distance of 6.0 kpc. Withthis distance, the system N36 is found to be situated at the interface of theGalactic bar and the Norma Galactic arm in our Galaxy, where one may expect thecollisions 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. Thesystem contains 27 ATLASGAL dust clumps at 870 micron. Several clumps aremassive (> 10^3 M_sun), and have high bolometric luminosity (> 10^3 L_sun).Using the GRS 13CO line data, in the direction of the system N36, two velocitycomponents are found around 109 and 113 km/s, and are linked in the velocityspace. The morphological analysis of 13CO favours the presence of interactingmolecular clouds in the system. Four H II regions and two 6.7 GHz masers arespatially observed at the common areas of the two clouds. The analysis of theSpitzer photometric data also traces the noticeable SF activity in the system.Considering the observational outcomes, the formation of O-type stars(including ongoing SF) in the system appears to be triggered by the collisionsof molecular clouds at the bar-arm interface.

The study of a system of H II regions toward l = 24.8 deg, b = 0.1 deg at the Galactic bar - Norma arm interface