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dc.contributor.authorElmegreen, Bruce G.
dc.contributor.authorKaufman, Michele
dc.contributor.authorBournaud, Frederic
dc.contributor.authorElmegreen, Debra Meloy
dc.contributor.authorStruck, Curtis
dc.contributor.authorBrinks, E.
dc.contributor.authorJuneau, Stephanie
dc.date.accessioned2017-01-11T20:24:27Z
dc.date.available2017-01-11T20:24:27Z
dc.date.issued2016-05-20
dc.identifier.citationElmegreen , B G , Kaufman , M , Bournaud , F , Elmegreen , D M , Struck , C , Brinks , E & Juneau , S 2016 , ' High star formation rates in turbulent atomic-dominated gas in the interacting galaxies IC 2163 and NGC 2207 ' , The Astrophysical Journal , vol. 823 , no. 1 . https://doi.org/10.3847/0004-637X/823/1/26
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 10010692
dc.identifier.otherPURE UUID: a46363a8-89b3-4a23-9317-335e83d7192f
dc.identifier.otherArXiv: http://arxiv.org/abs/1603.04533v1
dc.identifier.otherScopus: 84971659172
dc.identifier.otherORCID: /0000-0002-7758-9699/work/30407787
dc.identifier.urihttp://hdl.handle.net/2299/17483
dc.descriptionThis is a pre-copyedited, author produced PDF of an article accepted for publication in The Astrophysical Journal following peer review. The version of record (The Astrophysical Journal, 823:26, 2016 May 18) is available on line at doi:10.3847/0004-637X/823/1/26 © 2016. The American Astronomical Society. All rights reserved.
dc.description.abstractCO observations of the interacting galaxies IC 2163 and NGC 2207 are combined with HI, Halpha and 24 microns to study the star formation rate (SFR) surface density as a function of the gas surface density. More than half of the high SFR regions are HI dominated. When compared to other galaxies, these HI-dominated regions have excess SFRs relative to their molecular gas surface densities but normal SFRs relative to their total gas surface densities. The HI-dominated regions are mostly located in the outer part of NGC 2207, where the HI velocity dispersion is high, 40 - 50 km/s. We suggest that the star-forming clouds in these regions have envelopes at lower densities than normal, making them predominantly atomic, and cores at higher densities than normal because of the high turbulent Mach numbers. This is consistent with theoretical predictions of a flattening in the density probability distribution function for compressive, high Mach number turbulence.en
dc.format.extent7
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.subjectastro-ph.GA
dc.subjectISM : molecules
dc.subjectGalaxies: interactions
dc.subjectgalaxies: star formation
dc.titleHigh star formation rates in turbulent atomic-dominated gas in the interacting galaxies IC 2163 and NGC 2207en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.3847/0004-637X/823/1/26
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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