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We studied the environment of the dust bubble N10 in molecular emission.Infrared bubbles, first detected by the GLIMPSE survey at 8.0 $\mu$m, are idealregions to investigate the effect of the expansion of the HII region on itssurroundings eventual triggered star formation at its borders. In this work, wepresent a multi-wavelength study of N10. This bubble is especially interestingas infrared studies of the young stellar content suggest a scenario of ongoingstar formation, possibly triggered, on the edge of the HII region. We carriedout observations of $^{12}$CO(1-0) and $^{13}$CO(1-0) emission at PMO 13.7-mtowards N10. We also analyzed the IR and sub-mm emission on this region andcompare those different tracers to obtain a detailed view of the interactionbetween the expanding HII region and the molecular gas. We also estimated theparameters of the denser cold dust condensation and of the ionized gas insidethe shell. Bright CO emission was detected and two molecular clumps wereidentified, from which we have derived physical parameters. We also estimatethe parameters for the densest cold dust condensation and for the ionized gasinside the shell. The comparison between the dynamical age of this region andthe fragmentation time scale favors the "Radiation-Driven Implosion" mechanismof star formation. N10 reveals to be specially interesting case with gasstructures in a narrow frontier between HII region and surrounding molecularmaterial, and with a range of ages of YSOs situated in region indicatingtriggered star formation.

CO observations and investigation of triggered star formation towards N10 infrared bubble and surroundings