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dc.contributor.authorLoveday, J.
dc.contributor.authorNorberg, P.
dc.contributor.authorBaldry, I.K.
dc.contributor.authorBaldryBland-Hawthorn, J.
dc.contributor.authorBrough, S.
dc.contributor.authorBrown, M.J.I.
dc.contributor.authorDriver, S.P.
dc.contributor.authorKelvin, L.S.
dc.contributor.authorPhillipps, S.
dc.date.accessioned2015-08-13T12:10:01Z
dc.date.available2015-08-13T12:10:01Z
dc.date.issued2015-08-01
dc.identifier.citationLoveday , J , Norberg , P , Baldry , I K , BaldryBland-Hawthorn , J , Brough , S , Brown , M J I , Driver , S P , Kelvin , L S & Phillipps , S 2015 , ' Galaxy and Mass assembly (GAMA) : maximum-likelihood determination of the luminosity function and its evolution ' , Monthly Notices of the Royal Astronomical Society , vol. 451 , no. 2 , pp. 1540-1552 . https://doi.org/10.1093/mnras/stv1013en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 209421304
dc.identifier.otherPURE UUID: 50151d93-bed7-4a32-83f2-d3a5f70762ad
dc.identifier.otherScopus: 84938118195
dc.identifier.otherWOS: 000360830000032
dc.identifier.urihttp://hdl.handle.net/10023/7212
dc.descriptionJL acknowledges support from the Science and Technology Facilities Council (grant number ST/I000976/1) and illuminating discussions with Shaun Cole. PN acknowledges the support of the Royal Society through the award of a University Research Fellowship, the European Research Council, through receipt of a Starting Grant (DEGAS-259586) and the Science and Technology Facilities Council (ST/L00075X/1).en
dc.description.abstractWe describe modifications to the joint stepwise maximum-likelihood method of Cole in order to simultaneously fit the Galaxy and Mass Assembly II galaxy luminosity function (LF), corrected for radial density variations, and its evolution with redshift. The whole sample is reasonably well fitted with luminosity (Qe) and density (Pe) evolution parameters Qe, Pe ≈ 1.0, 1.0 but with significant degeneracies characterized by Qe ≈ 1.4 − 0.4Pe. Blue galaxies exhibit larger luminosity density evolution than red galaxies, as expected. We present the evolution-corrected r-band LF for the whole sample and for blue and red subsamples, using both Petrosian and Sérsic magnitudes. Petrosian magnitudes miss a substantial fraction of the flux of de Vaucouleurs profile galaxies: the Sérsic LF is substantially higher than the Petrosian LF at the bright end.
dc.format.extent13
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.en
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: luminosity function, mass functionen
dc.subjectGalaxies: statisticsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleGalaxy and Mass assembly (GAMA) : maximum-likelihood determination of the luminosity function and its evolutionen
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/stv1013
dc.description.statusPeer revieweden


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