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dc.contributor.authorBrindle, C.
dc.contributor.authorHough, J.
dc.contributor.authorBailey, J.
dc.contributor.authorAxon, D.J.
dc.contributor.authorSparks, W.
dc.identifier.citationBrindle , C , Hough , J , Bailey , J , Axon , D J & Sparks , W 1991 , ' An optical and near-infrared polarization survey of nearby starburst and interacting galaxies ' , Monthly Notices of the Royal Astronomical Society , vol. 252 , no. 2 , pp. 288-299 .
dc.identifier.otherPURE: 153322
dc.identifier.otherPURE UUID: 95174aae-6081-4a04-a164-dc63c877ac02
dc.identifier.otherdspace: 2299/3193
dc.identifier.otherScopus: 0040866381
dc.descriptionCopyright Royal Astronomical Society [Full text of this article is not available in the UHRA]
dc.description.abstractBroadband optical and near-infrared polarization and flux density measurements of a sample of 27 starburst and interacting galaxies are presented. The observed polarizations are generally small (P is less than 1 percent) and decrease with increasing wavelength. For those galaxies with significant polarization, the polarization E vector is usually parallel to a dust lane. The most likely polarization mechanism is the transmission of radiation through aligned dust grains lying in the plane of the galaxy. In some cases scattering by dust grains may contribute to the polarization. NGC 253 shows high polarization (4.3 percent in the V band), with a strong wavelength-dependence resembling a Serkowski curve having a small value of lambda(max) (0.34 micron). Modeling shows that this wavelength-dependence can also be produced by light polarized according to the Serkowski formula with a normal value of lambda(max) (0.55 micron) combined with unpolarized light with a redder spectrum.en
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.titleAn optical and near-infrared polarization survey of nearby starburst and interacting galaxiesen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.typeJournal Article/Review

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