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We studied the cloud-cloud collision candidate G323.18+0.15 based onsignatures of induced filaments, clumps, and star formation. We used archivalmolecular spectrum line data from the SEDIGISM $^{13}$CO($J$\,=\,2--1) survey,from the Mopra southern Galactic plane CO survey, and infrared to radio datafrom the GLIMPSE, MIPS, Hi-GAL, and SGPS surveys. Our new result shows that theG323.18+0.15 complex is 3.55kpc away from us and consists of three cloudcomponents, G323.18a, G323.18b, and G323.18c. G323.18b shows a perfect U-shapestructure, which can be fully complemented by G323.18a, suggesting a collisionbetween G323.18a and the combined G323.18bc filamentary structure. One densecompressed layer (filament) is formed at the bottom of G323.18b, where wedetect a greatly increased velocity dispersion. The bridge with an intermediatevelocity in a position-velocity diagram appears between G323.18a and G323.18b,which corresponds to the compressed layer. G323.18a plus G323.18b as a wholeare probably not gravitationally bound. This indicates that high-mass starformation in the compressed layer may have been caused by an accidental event.The column density in the compressed layer of about $1.36 \times10^{22}$cm$^{-2}$ and most of the dense clumps and high-mass stars are locatedthere. The average surface density of classI and classII young stellar objects(YSOs) inside the G323.18+0.15 complex is much higher than the density in thesurroundings. The timescale of the collision between G323.18a and G323.18b is$1.59$Myr. This is longer than the typical lifetime of classI YSOs and iscomparable to the lifetime of classII YSOs.

Cloud-cloud collision and star formation in G323.18+0.15