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Aiming at studying the physical properties of Galactic IR bubbles and toexplore their impact in triggering massive star formation, we perform amultiwavelength analysis of the bubble HII region Sh2-39 (N5) and its environs.To analyze the molecular gas we use CO(3-2) and HCO+(4-3) line data obtainedwith the ASTE telescope. To study the physical characteristics of the dust, wemake use of archival data from ATLASGAL, Herschel, and MSX, while the ionizedgas was studied making use of NVSS data. We use public IR point source catalogsto search for candidate YSOs in the region. To investigate the stellar cluster[BDS2003]6 we use IR spectroscopic data obtained with the ARCoIRISspectrograph, and new available IR Ks band observations from VVVX survey. Thenew ASTE observations allowed the molecular gas component in the velocity rangefrom 30 km/s to 46 km/s, associated with Sh2-39, to be studied in detail. Wehave identified four molecular clumps, that were likely formed by the expansionof the ionization front, and determined some of their physical and dynamicalproperties. Clumps having HCO+ and 870 micron counterparts show evidence ofgravitational collapse. We identified several candidate YSOs across themolecular component. Their spatial distribution, as well as the fragmentationtime derived for the collected layers of the molecular gas, suggest thatmassive star formation might have been triggered by the expansion of the nebulavia the collect and collapse mechanism. The spectroscopical distance obtainedfor the stellar cluster [BDS2003]6, placed over one of the collapsing clumps,reveals that this cluster is physically associated with the neabula and givesmore support to the triggered massive star formation scenario. A radiocontinuum data analysis indicates that the nebula is older and expands at lowervelocity than typical Galactic IR bubbles.

Triggered massive star formation associated with the bubble HII region Sh2-39 (N5)