%0 Generic %1 palmeirim2017spatial %A Palmeirim, P. %A Zavagno, A. %A Elia, D. %A Moore, T. J. T. %A Whitworth, A. %A Tremblin, P. %A Traficante, A. %A Merello, M. %A Russeil, D. %A Pezzuto, S. %A Cambrésy, L. %A Baldeschi, A. %A Bandieramonte, M. %A Becciani, U. %A Benedettini, M. %A Buemi, C. %A Bufano, F. %A Bulpitt, A. %A Butora, R. %A Carey, D. %A Costa, A. %A Deharveng, L. %A Di Giorgio, A. %A Eden, D. %A Hajnal, A. %A Hoare, M. %A Kacsuk, P. %A Leto, P. %A Marsh, K. %A Mège, P. %A Molinari, S. %A Molinaro, M. %A Noriega-Crespo, A. %A Schisano, E. %A Sciacca, E. %A Trigilio, C. %A Umana, G. %A Vitello, F. %D 2017 %K Galactic HII plane regions %T Spatial distribution of star formation related to ionized regions throughout the inner Galactic plane %U http://arxiv.org/abs/1705.09877 %X We present a comprehensive statistical analysis of star-forming objects located in the vicinities of 1 360 bubble structures throughout the Galactic Plane and their local environments. The compilation of ~70 000 star-forming sources, found in the proximity of the ionized (Hii) regions and detected in both Hi-GAL and GLIMPSE surveys, provided a broad overview of the different evolutionary stages of star-formation in bubbles, from prestellar objects to more evolved young stellar objects (YSOs). Surface density maps of star-forming objects clearly reveal an evolutionary trend where more evolved star-forming objects are found spatially located near the center, while younger star-forming objects are found at the edge of the bubbles. We derived dynamic ages for a subsample of 182 Hii regions for which kinematic distances and radio continuum flux measurements were available. We detect ~80% more star-forming sources per unit area in the direction of bubbles than in the surrounding fields. We estimate ~10% clump formation efficiency (CFE) of Hi-GAL clumps in bubbles, twice the CFE in fields not affected by feedback. We find higher CFE of protostellar clumps in younger bubbles, whose density of the bubble shells is higher. We argue that the formation rate from prestellar to protostellar phase is probably higher during the early stages of the bubble expansion. Evaluation of the fragmentation time inside the shell of bubbles advocates the preexistence of clumps in the medium before the bubble, as supported by numerical simulations. Approximately 23% of the Hi-GAL clumps are found located in the direction of a bubble, with 15% for prestellar clumps and 41% for protostellar clumps. We argue that the high fraction of protostellar clumps may be due to the acceleration of the star-formation process cause by the feedback of the (Hii) bubbles.

@misc{palmeirim2017spatial, abstract = {We present a comprehensive statistical analysis of star-forming objects located in the vicinities of 1 360 bubble structures throughout the Galactic Plane and their local environments. The compilation of ~70 000 star-forming sources, found in the proximity of the ionized (Hii) regions and detected in both Hi-GAL and GLIMPSE surveys, provided a broad overview of the different evolutionary stages of star-formation in bubbles, from prestellar objects to more evolved young stellar objects (YSOs). Surface density maps of star-forming objects clearly reveal an evolutionary trend where more evolved star-forming objects are found spatially located near the center, while younger star-forming objects are found at the edge of the bubbles. We derived dynamic ages for a subsample of 182 Hii regions for which kinematic distances and radio continuum flux measurements were available. We detect ~80% more star-forming sources per unit area in the direction of bubbles than in the surrounding fields. We estimate ~10% clump formation efficiency (CFE) of Hi-GAL clumps in bubbles, twice the CFE in fields not affected by feedback. We find higher CFE of protostellar clumps in younger bubbles, whose density of the bubble shells is higher. We argue that the formation rate from prestellar to protostellar phase is probably higher during the early stages of the bubble expansion. Evaluation of the fragmentation time inside the shell of bubbles advocates the preexistence of clumps in the medium before the bubble, as supported by numerical simulations. Approximately 23% of the Hi-GAL clumps are found located in the direction of a bubble, with 15% for prestellar clumps and 41% for protostellar clumps. We argue that the high fraction of protostellar clumps may be due to the acceleration of the star-formation process cause by the feedback of the (Hii) bubbles.}, added-at = {2017-05-30T09:52:56.000+0200}, author = {Palmeirim, P. and Zavagno, A. and Elia, D. and Moore, T. J. T. and Whitworth, A. and Tremblin, P. and Traficante, A. and Merello, M. and Russeil, D. and Pezzuto, S. and Cambrésy, L. and Baldeschi, A. and Bandieramonte, M. and Becciani, U. and Benedettini, M. and Buemi, C. and Bufano, F. and Bulpitt, A. and Butora, R. and Carey, D. and Costa, A. and Deharveng, L. and Di Giorgio, A. and Eden, D. and Hajnal, A. and Hoare, M. and Kacsuk, P. and Leto, P. and Marsh, K. and Mège, P. and Molinari, S. and Molinaro, M. and Noriega-Crespo, A. and Schisano, E. and Sciacca, E. and Trigilio, C. and Umana, G. and Vitello, F.}, biburl = {https://www.bibsonomy.org/bibtex/20bf113ac5841f133bb5186a7e262ddac/miki}, description = {[1705.09877] Spatial distribution of star formation related to ionized regions throughout the inner Galactic plane}, interhash = {98c7342060885f8ac1da74f54929fe05}, intrahash = {0bf113ac5841f133bb5186a7e262ddac}, keywords = {Galactic HII plane regions}, note = {cite arxiv:1705.09877Comment: 15 pages, 12 figures. Accepted for publication by Astronomy and Astrophysics}, timestamp = {2017-05-30T09:52:56.000+0200}, title = {Spatial distribution of star formation related to ionized regions throughout the inner Galactic plane}, url = {http://arxiv.org/abs/1705.09877}, year = 2017 }