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dc.contributor.authorGrootes, M.W.
dc.contributor.authorTuffs, R. J.
dc.contributor.authorPopescu, C. C.
dc.contributor.authorRobotham, A. S. G.
dc.contributor.authorSeibert, M.
dc.contributor.authorKelvin, L. S.
dc.date.accessioned2014-09-09T13:31:03Z
dc.date.available2014-09-09T13:31:03Z
dc.date.issued2014-02-01
dc.identifier.citationGrootes , M W , Tuffs , R J , Popescu , C C , Robotham , A S G , Seibert , M & Kelvin , L S 2014 , ' Non-parametric cell-based photometric proxies for galaxy morphology : methodology and application to the morphologically defined star formation-stellar mass relation of spiral galaxies in the local universe ' , Monthly Notices of the Royal Astronomical Society , vol. 437 , no. 4 , pp. 3883-3917 . https://doi.org/10.1093/mnras/stt2184en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 147007605
dc.identifier.otherPURE UUID: eea81512-ccb7-4277-a3ce-60f871d33fb2
dc.identifier.otherScopus: 84891364247
dc.identifier.otherWOS: 000329177100069
dc.identifier.urihttp://hdl.handle.net/10023/5396
dc.description.abstractWe present a non-parametric cell-based method of selecting highly pure and largely complete samples of spiral galaxies using photometric and structural parameters as provided by standard photometric pipelines and simple shape fitting algorithms. The performance of the method is quantified for different parameter combinations, using purely human-based classifications as a benchmark. The discretization of the parameter space allows a markedly superior selection than commonly used proxies relying on a fixed curve or surface of separation. Moreover, we find structural parameters derived using passbands longwards of the g band and linked to older stellar populations, especially the stellar mass surface density μ* and the r-band effective radius re, to perform at least equally well as parameters more traditionally linked to the identification of spirals by means of their young stellar populations, e.g. UV/optical colours. In particular, the distinct bimodality in the parameter μ*, consistent with expectations of different evolutionary paths for spirals and ellipticals, represents an often overlooked yet powerful parameter in differentiating between spiral and non-spiral/elliptical galaxies. We use the cell-based method for the optical parameter set including re in combination with the Sérsic index n and the i-band magnitude to investigate the intrinsic specific star formation rate-stellar mass relation (ψ*-M*) for a morphologically defined volume-limited sample of local Universe spiral galaxies. The relation is found to be well described by ψ* α M*-0.5over the range of 109.5 ≤ M* ≤ 1011M⊙ with a mean interquartile range of 0.4 dex. This is somewhat steeper than previous determinations based on colour-selected samples of starforming galaxies, primarily due to the inclusion in the sample of red quiescent discs.
dc.format.extent35
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectGalaxies: fundamental parametersen
dc.subjectGalaxes: photometryen
dc.subjectGalaxies: spiralen
dc.subjectGalaxies: structureen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleNon-parametric cell-based photometric proxies for galaxy morphology : methodology and application to the morphologically defined star formation-stellar mass relation of spiral galaxies in the local universeen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stt2184
dc.description.statusPeer revieweden
dc.identifier.urlhttp://mnras.oxfordjournals.org/content/437/4/3883/suppl/DC1en


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