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dc.contributor.authorLouvet, F.
dc.contributor.authorMotte, F.
dc.contributor.authorHennebelle, P.
dc.contributor.authorMaury, A.
dc.contributor.authorBonnell, I.
dc.contributor.authorBontemps, S.
dc.contributor.authorGusdorf, A.
dc.contributor.authorHill, T.
dc.contributor.authorGueth, F.
dc.contributor.authorPeretto, N.
dc.contributor.authorDuarte-Cabral, A.
dc.contributor.authorStephan, G.
dc.contributor.authorSchilke, P.
dc.contributor.authorCsengeri, T.
dc.contributor.authorLuong, Q. Nguyen
dc.contributor.authorLis, D. C.
dc.date.accessioned2014-12-04T15:31:10Z
dc.date.available2014-12-04T15:31:10Z
dc.date.issued2014-10
dc.identifier.citationLouvet , F , Motte , F , Hennebelle , P , Maury , A , Bonnell , I , Bontemps , S , Gusdorf , A , Hill , T , Gueth , F , Peretto , N , Duarte-Cabral , A , Stephan , G , Schilke , P , Csengeri , T , Luong , Q N & Lis , D C 2014 , ' The W43-MM1 mini-starburst ridge, a test for star formation efficiency models ' , Astronomy & Astrophysics , vol. 570 , 15 . https://doi.org/10.1051/0004-6361/201423603en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 158990119
dc.identifier.otherPURE UUID: e47ba0b9-a1bd-4e42-8a72-75a1fdcabfb9
dc.identifier.otherWOS: 000344158500029
dc.identifier.otherScopus: 84907831019
dc.identifier.otherWOS: 000344158500029
dc.identifier.urihttp://hdl.handle.net/10023/5870
dc.description.abstractContext. Star formation efficiency (SFE) theories are currently based on statistical distributions of turbulent cloud structures and a simple model of star formation from cores. They remain poorly tested, especially at the highest densities. Aims. We investigate the effects of gas density on the SFE through measurements of the core formation efficiency (CFE). With a total mass of similar to 2 x 104 M⊙, the W43-MM1 ridge is one of the most convincing candidate precursors of Galactic starburst clusters and thus one of the best places to investigate star formation. Methods. We used high-angular resolution maps obtained at 3 mm and 1 mm within the W43-MM1 ridge with the IRAM Plateau de Bure Interferometer to reveal a cluster of 11 massive dense cores, and, one of the most massive protostellar cores known. A Herschel column density image provided the mass distribution of the cloud gas. We then measured the "instantaneous" CFE and estimated the SFE and the star formation rate (SFR) within subregions of the W43-MM1 ridge. Results. The high SFE found in the ridge (~ 6% enclosed in ~ 8 pc3) confirms its ability to form a starburst cluster. There is, however, a clear lack of dense cores in the eastern part of the ridge, which may be currently assembling. The CFE and the SFE are observed to increase with volume gas density, while the SFR per free fall time steeply decreases with the virial parameter, αvir. Statistical models of the SFR may describe the outskirts of the W43-MM1 ridge well, but struggle to reproduce its inner part, which corresponds to measurements at low αvir. It may be that ridges do not follow the log-normal density distribution, Larson relations, and stationary conditions forced in the statistical SFR models.
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rightsReproduced with permission from Astronomy & Astrophysics, © ESOen
dc.subjectstars: formationen
dc.subjectstars: protostarsen
dc.subjectstars: massiveen
dc.subjectISM: cloudsen
dc.subjectsubmillimeter: ISMen
dc.subjectsubmillimeter: starsen
dc.subjectNearby molecular cloudsen
dc.subjectYoung stellar objectsen
dc.subjectG30.79 FIR 10en
dc.subjectCYGNUS-Xen
dc.subjectInitial-highlightsen
dc.subjectMassive protostarsen
dc.subjectPrestellar coresen
dc.subjectEarliest phasesen
dc.subjectMagnetic-fieldsen
dc.subjectForming complexen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe W43-MM1 mini-starburst ridge, a test for star formation efficiency modelsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201423603
dc.description.statusPeer revieweden


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