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dc.contributor.authorLin, Y.
dc.contributor.authorLiu, H.~B.
dc.contributor.authorLi, D.
dc.contributor.authorZhang, Z.-Y.
dc.contributor.authorGinsburg, A.
dc.contributor.authorPineda, J.~E.
dc.contributor.authorQian, L.
dc.contributor.authorGalván-Madrid, R.
dc.contributor.authorMcLeod, A.~F.
dc.contributor.authorRosolowsky, E.
dc.contributor.authorDale, James
dc.contributor.authorImmer, K.
dc.contributor.authorKoch, E.
dc.contributor.authorLongmore, S.
dc.contributor.authorTesti, L.
dc.contributor.authorWalker, D
dc.date.accessioned2016-12-12T18:38:14Z
dc.date.available2016-12-12T18:38:14Z
dc.date.issued2016-09-01
dc.identifier.citationLin , Y , Liu , H B , Li , D , Zhang , Z-Y , Ginsburg , A , Pineda , J E , Qian , L , Galván-Madrid , R , McLeod , A F , Rosolowsky , E , Dale , J , Immer , K , Koch , E , Longmore , S , Testi , L & Walker , D 2016 , ' Cloud Structure of Galactic OB Cluster-forming Regions from Combining Ground- and Space-based Bolometric Observations ' , The Astrophysical Journal , vol. 828 , pp. 32 . https://doi.org/10.3847/0004-637X/828/1/32
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 10626903
dc.identifier.otherPURE UUID: 0b203f33-11fe-48b9-a605-8f8091dceacd
dc.identifier.otherBibtex: urn:3f213768c694320408d2e490b995af94
dc.identifier.otherScopus: 84987713294
dc.identifier.otherORCID: /0000-0001-5252-5771/work/62751060
dc.identifier.urihttp://hdl.handle.net/2299/17414
dc.descriptionThe final, definitive version of this paper has been published in The Astrophysical Journal, 828:32 (50pp), 1 September 2016, © 2016, doi: 10.3847/0004-637X/828/1/32, first published on line August 25, 2016, by the The American Astronomical Society. All rights reserved.
dc.description.abstractWe have developed an iterative procedure to systematically combine the millimeter and submillimeter images of OB cluster-forming molecular clouds, which were taken by ground-based (CSO, JCMT, APEX, and IRAM-30 m) and space telescopes (Herschel and Planck). For the seven luminous ($L\gt {10}^{6}$ L ⊙) Galactic OB cluster-forming molecular clouds selected for our analyses, namely W49A, W43-Main, W43-South, W33, G10.6-0.4, G10.2-0.3, and G10.3-0.1, we have performed single-component, modified blackbody fits to each pixel of the combined (sub)millimeter images, and the Herschel PACS and SPIRE images at shorter wavelengths. The ~10'' resolution dust column density and temperature maps of these sources revealed dramatically different morphologies, indicating very different modes of OB cluster-formation, or parent molecular cloud structures in different evolutionary stages. The molecular clouds W49A, W33, and G10.6-0.4 show centrally concentrated massive molecular clumps that are connected with approximately radially orientated molecular gas filaments. The W43-Main and W43-South molecular cloud complexes, which are located at the intersection of the Galactic near 3 kpc (or Scutum) arm and the Galactic bar, show a widely scattered distribution of dense molecular clumps/cores over the observed ~10 pc spatial scale. The relatively evolved sources G10.2-0.3 and G10.3-0.1 appear to be affected by stellar feedback, and show a complicated cloud morphology embedded with abundant dense molecular clumps/cores. We find that with the high angular resolution we achieved, our visual classification of cloud morphology can be linked to the systematically derived statistical quantities (i.e., the enclosed mass profile, the column density probability distribution function (N-PDF), the two-point correlation function of column density, and the probability distribution function of clump/core separations). In particular, the massive molecular gas clumps located at the center of G10.6-0.4 and W49A, which contribute to a considerable fraction of their overall cloud masses, may be special OB cluster-forming environments as a direct consequence of global cloud collapse. These centralized massive molecular gas clumps also uniquely occupy much higher column densities than what is determined by the overall fit of power-law N-PDF. We have made efforts to archive the derived statistical quantities of individual target sources, to permit comparisons with theoretical frameworks, numerical simulations, and other observations in the future.target sources, to permit comparisons with theoretical frameworks, numerical simulations, and otheren
dc.format.extent1
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.subjectISM: structure, methods: statistical, stars: formation, submillimeter: ISM, techniques: image processing
dc.titleCloud Structure of Galactic OB Cluster-forming Regions from Combining Ground- and Space-based Bolometric Observationsen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.3847/0004-637X/828/1/32
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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