Herschel Observations of the W3 GMC (II): Clues to the Formation of Clusters of High-Mass Stars
| dc.contributor.author | RIVERA-INGRAHAM, A., | |
| hal.structure.identifier | Department of Applied Mathematics and Statistics, | |
| dc.contributor.author | MARTIN, P. G., | |
| dc.contributor.author | POLYCHRONI, D., | |
| hal.structure.identifier | FORMATION STELLAIRE 2015 | |
| dc.contributor.author | SCHNEIDER, N. | |
| dc.contributor.author | MOTTE, F., | |
| hal.structure.identifier | FORMATION STELLAIRE 2015 | |
| dc.contributor.author | BONTEMPS, Sylvain | |
| hal.structure.identifier | Astrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)] | |
| dc.contributor.author | HENNEMANN, M. | |
| dc.contributor.author | MEN'SHCHIKOV, A., | |
| dc.contributor.author | NGUYEN LUONG, Q., | |
| hal.structure.identifier | Laboratoire d'Astrophysique de Marseille [LAM] | |
| dc.contributor.author | ZAVAGNO, Annie | |
| dc.contributor.author | ANDRE, Ph., | |
| dc.contributor.author | BERNARD, J.-Ph., | |
| dc.contributor.author | DI FRANCESCO, J., | |
| dc.contributor.author | FALLSCHEER, C., | |
| dc.contributor.author | HILL, T., | |
| dc.contributor.author | KONYVES, V., | |
| dc.contributor.author | MARSTON, A., | |
| dc.contributor.author | PEZZUTO, S., | |
| dc.contributor.author | RYGL, . K. L. J., | |
| dc.contributor.author | SPINOGLIO, L., | |
| hal.structure.identifier | SLAC National Accelerator Laboratory [SLAC] | |
| dc.contributor.author | WHITE, G. J., | |
| dc.date.issued | 2015-07 | |
| dc.identifier.issn | 0004-637X | |
| dc.description.abstractEn | The W3 GMC is a prime target for investigating the formation of high-mass stars and clusters. This second study of W3 within the HOBYS Key Program provides a comparative analysis of subfields within W3 to further constrain the processes leading to the observed structures and stellar population. Probability density functions (PDFs) and cumulative mass distributions (CMDs) were created from dust column density maps, quantified as extinction Av. The shape of the PDF, typically represented with a lognormal function at low Av "breaking" to a power-law tail at high Av, is influenced by various processes including turbulence and self-gravity. The breaks can also be identified, often more readily, in the CMDs. The PDF break from lognormal (Av(SF)= 6-10 mag) appears to shift to higher Av by stellar feedback, so that high-mass star-forming regions tend to have higher PDF breaks. A second break at Av > 50 mag traces structures formed or influenced by a dynamic process. Because such a process has been suggested to drive high-mass star formation in W3, this second break might then identify regions with potential for hosting high-mass stars/clusters. Stellar feedback appears to be a major mechanism driving the local evolution and state of regions within W3. A high initial star formation efficiency in a dense medium could result in a self-enhancing process, leading to more compression and favourable star-formation conditions (e.g., colliding flows), a richer stellar content, and massive stars. This scenario would be compatible with the "convergent constructive feedback" model introduced in our previous Herschel study. | |
| dc.language.iso | en | |
| dc.publisher | American Astronomical Society | |
| dc.subject.en | Astrophysics - Astrophysics of Galaxies | |
| dc.title.en | Herschel Observations of the W3 GMC (II): Clues to the Formation of Clusters of High-Mass Stars | |
| dc.type | Article de revue | |
| dc.identifier.doi | 10.1088/0004-637X/809/1/81 | |
| dc.subject.hal | Planète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO] | |
| dc.identifier.arxiv | 1507.02055 | |
| bordeaux.journal | The Astrophysical Journal | |
| bordeaux.page | id. 81 | |
| bordeaux.volume | 809 | |
| bordeaux.issue | 1 | |
| bordeaux.peerReviewed | oui | |
| hal.identifier | hal-01174415 | |
| hal.version | 1 | |
| hal.popular | non | |
| hal.audience | Internationale | |
| hal.origin.link | https://hal.archives-ouvertes.fr//hal-01174415v1 | |
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