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dc.contributor.authorKnapen, J.
dc.date.accessioned2008-02-05T12:10:43Z
dc.date.available2008-02-05T12:10:43Z
dc.date.issued1997
dc.identifier.citationKnapen , J 1997 , ' Atomic hydrogen in the spiral galaxy NGC 3631 ' , Monthly Notices of the Royal Astronomical Society , vol. 286 , pp. 403- .
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 146863
dc.identifier.otherPURE UUID: eb9d1a2e-91a7-41df-966b-5a0f9caad586
dc.identifier.otherdspace: 2299/1557
dc.identifier.otherScopus: 0000247505
dc.identifier.urihttp://hdl.handle.net/2299/1557
dc.description.abstractNew high resolution, high sensitivity WSRT Hi synthesis observations of the spiral galaxy NGC 3631 are presented. In the total atomic hydrogen map, the spiral arms are well distinguished from the interarm regions, while the sensitivity allows detection of Hi in all but a few isolated regions of the areas between the spiral arms. Most of the atomic hydrogen is located within the optical disc, but the Hi extends to some 1.5×Ropt. The Hi follows the spiral arms, and streaming motions of up to ~ 15 kms−1 (projected) can be identified from the velocity field. Assuming a constant inclination angle of 17◦, a rotation curve is derived which is slightly falling in the outer parts of the disc. Analysis of a residual velocity field, obtained after subtraction of an axisymmetric model based on the rotation curve, confirms the existence of streaming motions near the spiral arms in an otherwise undisturbed disc.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.titleAtomic hydrogen in the spiral galaxy NGC 3631en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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