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We present a comprehensive statistical analysis of star-forming objectslocated in the vicinities of 1 360 bubble structures throughout the GalacticPlane and their local environments. The compilation of ~70 000 star-formingsources, found in the proximity of the ionized (Hii) regions and detected inboth Hi-GAL and GLIMPSE surveys, provided a broad overview of the differentevolutionary stages of star-formation in bubbles, from prestellar objects tomore evolved young stellar objects (YSOs). Surface density maps of star-formingobjects clearly reveal an evolutionary trend where more evolved star-formingobjects are found spatially located near the center, while younger star-formingobjects are found at the edge of the bubbles. We derived dynamic ages for asubsample of 182 Hii regions for which kinematic distances and radio continuumflux measurements were available. We detect ~80% more star-forming sources perunit area in the direction of bubbles than in the surrounding fields. Weestimate ~10% clump formation efficiency (CFE) of Hi-GAL clumps in bubbles,twice the CFE in fields not affected by feedback. We find higher CFE ofprotostellar clumps in younger bubbles, whose density of the bubble shells ishigher. We argue that the formation rate from prestellar to protostellar phaseis probably higher during the early stages of the bubble expansion. Evaluationof the fragmentation time inside the shell of bubbles advocates thepreexistence of clumps in the medium before the bubble, as supported bynumerical simulations. Approximately 23% of the Hi-GAL clumps are found locatedin the direction of a bubble, with 15% for prestellar clumps and 41% forprotostellar clumps. We argue that the high fraction of protostellar clumps maybe due to the acceleration of the star-formation process cause by the feedbackof the (Hii) bubbles.

Spatial distribution of star formation related to ionized regions throughout the inner Galactic plane