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We present a multi-wavelength analysis of the infrared dust bubble S24, andits environs, with the aim of investigating the characteristics of themolecular gas and the interstellar dust linked to them, and analyzing theevolutionary status of the young stellar objects (YSOs) identified there. UsingAPEX data, we mapped the molecular emission in the CO(2-1), $^{13}$CO(2-1),C$^{18}$O(2-1), and $^{13}$CO(3-2) lines in a region of about 5'x 5' in sizearound the bubble. The cold dust distribution was analyzed using ATLASGAL andHerschel images. Complementary IR and radio data were also used.The moleculargas linked to the S24 bubble, G341.220-0.213, and G341.217-0.237 has velocitiesbetween -48.0 km sec$^{-1}$ and -40.0 km sec$^{-1}$. The gas distributionreveals a shell-like molecular structure of $\sim$0.8 pc in radius borderingthe bubble. A cold dust counterpart of the shell is detected in the LABOCA andHerschel images.The presence of extended emission at 24 $\mu$m and radiocontinuum emission inside the bubble indicates that the bubble is a compact HIIregion. Part of the molecular gas bordering S24 coincides with the extendedinfrared dust cloud SDC341.194-0.221. A cold molecular clump is present at theinterface between S24 and G341.217-0.237. As regards G341.220-0.213, thepresence of an arc-like molecular structure at the northern and easternsections of this IR source indicates that G341.220-0.213 is interacting withthe molecular gas. Several YSO candidates are found to be linked to the IRextended sources, thus confirming their nature as active star-forming regions.The total gas mass in the region and the H$_2$ ambient density amount to 10300M$_{\odot}$ and 5900 cm$^{-3}$, indicating that G341.220-0.213, G341.217-0.237,and the S24 HII region are evolving in a high density medium. A triggering starformation scenario is also investigated.

Molecular gas and star formation towards the IR dust bubble S24 and its environs