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dc.contributor.authorKnapen, J.
dc.contributor.authorBeckman, J.E.
dc.date.accessioned2008-02-05T12:10:44Z
dc.date.available2008-02-05T12:10:44Z
dc.date.issued1996
dc.identifier.citationKnapen , J & Beckman , J E 1996 , ' Global morphology and physical relations between the stars, gas and dust in the disc and arms of M100 ' , Monthly Notices of the Royal Astronomical Society , vol. 283 , pp. 251-265 .
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 167657
dc.identifier.otherPURE UUID: 5145f654-25c3-423f-a317-800167fb3b54
dc.identifier.otherdspace: 2299/1558
dc.identifier.otherScopus: 0000260030
dc.identifier.urihttp://hdl.handle.net/2299/1558
dc.description.abstractWe study star formation processes in the disc of the weakly barred grand design spiral galaxy M100 (NGC 4321) from a variety of images tracing recent massive star formation, old and young stars, dust, and neutral hydrogen. Differences between arm and interarm regions are specifically studied by decomposing the images into arm and non-arm zones. We find from a comparison of the morphology in H , Hi and dust that while the first two are coincident over most of the disc, they are offset from the dust lanes especially along the inner parts of the spiral arms: a picture which is indicative of a density wave shock moving through the arms. Hi is formed near the young massive stars as a result of photo-dissociation. From radial profiles we find that in the region of the star-forming spiral arms the exponential scale lengths for H , blue and near-infrared light, and 21 cm radio continuum are equal within the fitting errors. The scale lengths for the interarm region are also equal for all these tracers, but the arm scale lengths are significantly longer. This points to a common origin of the profiles in star formation, with little or no influence from radial population gradients or dust in the disc of this galaxy. The longer arm scale lengths are equivalent to an outwardly increasing arm-interarm contrast.We argue that the radial profiles of radio continuum and Hi, as well as CO, are also directly regulated by star formation, and discuss the possible implications of this result for the interpretation of observed CO intensities in and outside spiral arms. We discuss the radial atomic hydrogen profile in some detail. Its almost perfectly flat shape in the region of the star-forming spiral arms may be explained by photodissociation and recombination processes in the presence of a limited quantity of interstellar dust, controlling the equilibrium between the molecular and atomic form of hydrogen. Over most of the inner part of the disc, Hi seems to be a product of the star formation processes, rather than the cause of enhanced star formation.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.titleGlobal morphology and physical relations between the stars, gas and dust in the disc and arms of M100en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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