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dc.contributor.authorEden, D. J.
dc.contributor.authorMoore, T. J.T.
dc.contributor.authorPlume, R.
dc.contributor.authorRigby, A. J.
dc.contributor.authorUrquhart, J. S.
dc.contributor.authorMarsh, K. A.
dc.contributor.authorPeñaloza, C. H.
dc.contributor.authorClark, P. C.
dc.contributor.authorSmith, M. W.L.
dc.contributor.authorTahani, K.
dc.contributor.authorRagan, S. E.
dc.contributor.authorThompson, M. A.
dc.contributor.authorJohnstone, D.
dc.contributor.authorParsons, H.
dc.contributor.authorRani, R.
dc.date.accessioned2020-12-23T17:30:12Z
dc.date.available2020-12-23T17:30:12Z
dc.date.issued2021-01
dc.identifier271799840
dc.identifier4ae16154-e43f-4dab-a6f5-b2b2034ef6ca
dc.identifier85097469961
dc.identifier000599134600015
dc.identifier.citationEden , D J , Moore , T J T , Plume , R , Rigby , A J , Urquhart , J S , Marsh , K A , Peñaloza , C H , Clark , P C , Smith , M W L , Tahani , K , Ragan , S E , Thompson , M A , Johnstone , D , Parsons , H & Rani , R 2021 , ' Characteristic scale of star formation – I. Clump formation efficiency on local scales ' , Monthly Notices of the Royal Astronomical Society , vol. 500 , no. 1 , pp. 191-210 . https://doi.org/10.1093/mnras/staa3188en
dc.identifier.issn0035-8711
dc.identifier.urihttps://hdl.handle.net/10023/21199
dc.descriptionFunding: DJE is supported by an STFC postdoctoral grant (ST/R000484/1).en
dc.description.abstractWe have used the ratio of column densities derived independently from the 850-μm continuum James Clerk Maxwell Telescope Plane Survey and the 13CO/C18O (J = 3 → 2) Heterodyne Inner Milky Way Plane Survey to produce maps of the dense-gas mass fraction (DGMF) in two slices of the Galactic plane centred at l= 30◦ and 40◦. The observed DGMF is a metric for the instantaneous clump formation efficiency (CFE) in the molecular gas. We split the two fields into velocity components corresponding to the spiral arms that cross them, and a two-dimensional power-spectrum analysis of the spiral-arm DGMF maps reveals a break in slope at the approximate size scale of molecular clouds. We interpret this as the characteristic scale of the amplitude of variations in the CFE and a constraint on the dominant mechanism regulating the CFE and, hence, the star formation efficiency in CO-traced clouds.
dc.format.extent20
dc.format.extent5748822
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.subjectISM: individual objects: W43en
dc.subjectISM: kinematics and dynamicsen
dc.subjectStars: formationen
dc.subjectSubmillimetre: ISMen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectAstronomy and Astrophysicsen
dc.subjectSpace and Planetary Scienceen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleCharacteristic scale of star formation – I. Clump formation efficiency on local scalesen
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doi10.1093/mnras/staa3188
dc.description.statusPeer revieweden


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