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dc.contributor.authorBarnes, A. T.
dc.contributor.authorLongmore, S. N.
dc.contributor.authorAvison, A.
dc.contributor.authorContreras, Y.
dc.contributor.authorGinsburg, A.
dc.contributor.authorHenshaw, J. D.
dc.contributor.authorRathborne, J. M.
dc.contributor.authorWalker, D. L.
dc.contributor.authorAlves, J.
dc.contributor.authorBally, J.
dc.contributor.authorBattersby, C.
dc.contributor.authorBeltrán, M. T.
dc.contributor.authorBeuther, H.
dc.contributor.authorGaray, G.
dc.contributor.authorGomez, L.
dc.contributor.authorJackson, J.
dc.contributor.authorKainulainen, J.
dc.contributor.authorKruijssen, J. M. D.
dc.contributor.authorLu, X.
dc.contributor.authorMills, Elisabeth
dc.contributor.authorOtt, J.
dc.contributor.authorPeters, T.
dc.date.accessioned2021-04-12T21:06:14Z
dc.date.available2021-04-12T21:06:14Z
dc.date.issued2019-03-19
dc.identifier.citationA T Barnes, S N Longmore, A Avison, Y Contreras, A Ginsburg, J D Henshaw, J M Rathborne, D L Walker, J Alves, J Bally, C Battersby, M T Beltrán, H Beuther, G Garay, L Gomez, J Jackson, J Kainulainen, J M D Kruijssen, X Lu, E A C Mills, J Ott, T Peters, Young massive star cluster formation in the Galactic Centre is driven by global gravitational collapse of high-mass molecular clouds, Monthly Notices of the Royal Astronomical Society, Volume 486, Issue 1, June 2019, Pages 283–303, https://doi.org/10.1093/mnras/stz796en_US
dc.identifier.urihttp://hdl.handle.net/1808/31591
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.en_US
dc.description.abstractYoung massive clusters (YMCs) are the most compact, high-mass stellar systems still forming at the present day. The precursor clouds to such systems are, however, rare due to their large initial gas mass reservoirs and rapid dispersal time-scales due to stellar feedback. None the less, unlike their high-z counterparts, these precursors are resolvable down to the sites of individually forming stars, and hence represent the ideal environments in which to test the current theories of star and cluster formation. Using high angular resolution (1 arcsec / 0.05 pc) and sensitivity ALMA observations of two YMC progenitor clouds in the Galactic Centre, we have identified a suite of molecular line transitions – e.g. c-C3H2 (7 − 6) – that are believed to be optically thin, and reliably trace the gas structure in the highest density gas on star-forming core scales. We conduct a virial analysis of the identified core and proto-cluster regions, and show that half of the cores (5/10) and both proto-clusters are unstable to gravitational collapse. This is the first kinematic evidence of global gravitational collapse in YMC precursor clouds at such an early evolutionary stage. The implications are that if these clouds are to form YMCs, then they likely do so via the ‘conveyor-belt’ mode, whereby stars continually form within dispersed dense gas cores as the cloud undergoes global gravitational collapse. The concurrent contraction of both the cluster-scale gas and embedded (proto-)stars ultimately leads to the high (proto-)stellar density in YMCs.en_US
dc.publisherRoyal Astronomical Societyen_US
dc.rights© 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.en_US
dc.titleYoung massive star cluster formation in the Galactic Centre is driven by global gravitational collapse of high-mass molecular cloudsen_US
dc.typeArticleen_US
kusw.kuauthorMills, Elisabeth
kusw.kudepartmentPhysics and Astronomyen_US
dc.identifier.doi10.1093/mnras/stz796en_US
dc.identifier.orcidhttps://orcid.org/0000-0003-0410-4504en_US
dc.identifier.orcidhttps://orcid.org/0000-0001-9656-7682en_US
dc.identifier.orcidhttps://orcid.org/0000-0002-4355-0921en_US
dc.identifier.orcidhttps://orcid.org/0000-0002-8804-0212en_US
dc.identifier.orcidhttps://orcid.org/0000-0001-8782-1992en_US
kusw.oaversionScholarly/refereed, publisher versionen_US
kusw.oapolicyThis item meets KU Open Access policy criteria.en_US
dc.rights.accessrightsopenAccessen_US


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