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Characteristic scale of star formation – I. Clump formation efficiency on local scales
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dc.contributor.author | Eden, D. J. | |
dc.contributor.author | Moore, T. J.T. | |
dc.contributor.author | Plume, R. | |
dc.contributor.author | Rigby, A. J. | |
dc.contributor.author | Urquhart, J. S. | |
dc.contributor.author | Marsh, K. A. | |
dc.contributor.author | Peñaloza, C. H. | |
dc.contributor.author | Clark, P. C. | |
dc.contributor.author | Smith, M. W.L. | |
dc.contributor.author | Tahani, K. | |
dc.contributor.author | Ragan, S. E. | |
dc.contributor.author | Thompson, M. A. | |
dc.contributor.author | Johnstone, D. | |
dc.contributor.author | Parsons, H. | |
dc.contributor.author | Rani, R. | |
dc.date.accessioned | 2020-12-23T17:30:12Z | |
dc.date.available | 2020-12-23T17:30:12Z | |
dc.date.issued | 2021-01 | |
dc.identifier | 271799840 | |
dc.identifier | 4ae16154-e43f-4dab-a6f5-b2b2034ef6ca | |
dc.identifier | 85097469961 | |
dc.identifier | 000599134600015 | |
dc.identifier.citation | Eden , 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/staa3188 | en |
dc.identifier.issn | 0035-8711 | |
dc.identifier.uri | https://hdl.handle.net/10023/21199 | |
dc.description | Funding: DJE is supported by an STFC postdoctoral grant (ST/R000484/1). | en |
dc.description.abstract | We 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.extent | 20 | |
dc.format.extent | 5748822 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en |
dc.subject | ISM: individual objects: W43 | en |
dc.subject | ISM: kinematics and dynamics | en |
dc.subject | Stars: formation | en |
dc.subject | Submillimetre: ISM | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | Astronomy and Astrophysics | en |
dc.subject | Space and Planetary Science | en |
dc.subject | 3rd-DAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Characteristic scale of star formation – I. Clump formation efficiency on local scales | en |
dc.type | Journal article | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.identifier.doi | https://doi.org/10.1093/mnras/staa3188 | |
dc.description.status | Peer reviewed | en |
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