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dc.contributor.authorTaylor, C.L.
dc.contributor.authorBrinks, E.
dc.contributor.authorPogge, R.
dc.contributor.authorSkillman, E.D.
dc.date.accessioned2009-01-09T13:42:04Z
dc.date.available2009-01-09T13:42:04Z
dc.date.issued1994
dc.identifier.citationTaylor , C L , Brinks , E , Pogge , R & Skillman , E D 1994 , ' Star formation thresholds in H II galaxies with H I companions ' , The Astronomical Journal , vol. 107 , no. 3 , pp. 971-983 . https://doi.org/10.1086/116910
dc.identifier.issn0004-6256
dc.identifier.otherPURE: 150119
dc.identifier.otherPURE UUID: d7dd00fe-0c0a-4ba2-9d0c-4080b3571646
dc.identifier.otherdspace: 2299/2783
dc.identifier.otherScopus: 0000668022
dc.identifier.otherORCID: /0000-0002-7758-9699/work/30407942
dc.identifier.urihttp://hdl.handle.net/2299/2783
dc.descriptionOriginal article can be found at: http://adsabs.harvard.edu/abs/ Copyright American Astronomical Society. DOI: 10.1086/116910 [Full text of this article is not available in the UHRA]
dc.description.abstractWe present high resolution Very Large Array (VLA) 21 cm line observations of five H II galaxies combined with previous lower resolution data from Taylor et al. (1993) and optical broadband R and H-alpha Charge Coupled Device (CCD) images of the systems. Following Kennicutt (1989) we calculated the threshold H I surface density for star formation for the H II galaxies and compared the location and shape of this predicted threshold density contour with the optical shape of the galaxies. We find generally a good correlation between these two, although a constant density contour of 1021/sq cm fits the images of the optical galaxies equally as well. The H I synthesis observations have revealed that the H II galaxies have sharply peaked H I radial profiles, in contrast to the relatively flattened profiles of low surface brightness (LSB) galaxies, suggesting that large central concentrations of gas are a necessary condition for the occurrence of bursts of massive star formation seen in H II galaxies. These observations are consistent with the hypothesis that LSB galaxies represent the quiescent phase of H II galaxies, if a suitable mechanism exists (such as galaxy interactions) to cause H I to concentrate at the center of LSB galaxies prior to the onset of the burst of star formation. However, it is noted that the H II galaxies (and dwarf galaxies in general) span a relatively large range in mass. Since many properties correlate with mass (e.g., gas mass fraction), we point out that great care needs to be taken in choosing the proper comparison samples of LSB and H II galaxies.en
dc.language.isoeng
dc.relation.ispartofThe Astronomical Journal
dc.titleStar formation thresholds in H II galaxies with H I companionsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1086/116910
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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