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dc.contributor.authorBremer, M. N.
dc.contributor.authorPhillipps, S.
dc.contributor.authorKelvin, L. S.
dc.contributor.authorPropris, R. De
dc.contributor.authorKennedy, Rebecca
dc.contributor.authorMoffett, Amanda J.
dc.contributor.authorBamford, S.
dc.contributor.authorDavies, L. J. M.
dc.contributor.authorDriver, S. P.
dc.contributor.authorHäußler, B.
dc.contributor.authorHolwerda, B.
dc.contributor.authorHopkins, A.
dc.contributor.authorJames, P. A.
dc.contributor.authorLiske, J.
dc.contributor.authorPercival, S.
dc.contributor.authorTaylor, E. N.
dc.date.accessioned2018-03-16T15:30:09Z
dc.date.available2018-03-16T15:30:09Z
dc.date.issued2018-05-01
dc.identifier.citationBremer , M N , Phillipps , S , Kelvin , L S , Propris , R D , Kennedy , R , Moffett , A J , Bamford , S , Davies , L J M , Driver , S P , Häußler , B , Holwerda , B , Hopkins , A , James , P A , Liske , J , Percival , S & Taylor , E N 2018 , ' Galaxy and Mass Assembly (GAMA) : morphological transformation of galaxies across the green valley ' , Monthly Notices of the Royal Astronomical Society , vol. 476 , no. 1 , pp. 12-26 . https://doi.org/10.1093/mnras/sty124en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 252572386
dc.identifier.otherPURE UUID: f57e5ee4-3433-45cd-bc5b-902cd574ce8f
dc.identifier.otherArXiv: http://arxiv.org/abs/1801.04277v1
dc.identifier.otherScopus: 85043505438
dc.identifier.otherWOS: 000429276700002
dc.identifier.urihttp://hdl.handle.net/10023/12964
dc.description.abstractWe explore constraints on the joint photometric and morphological evolution of typical low redshift galaxies as they move from the blue cloud through the green valley and on to the red sequence. We select Galaxy And Mass Assembly (GAMA) survey galaxies with 10.25 < log(M*/M⊙) < 10.75 and z < 0.2 classified according to their intrinsic u* − r* colour. From single component Sérsic fits, we find that the stellar mass-sensitive K-band profiles of red and green galaxy populations are very similar while g-band profiles indicate more disc-like morphologies for the green galaxies: apparent (optical) morphological differences arise primarily from radial mass-to-light ratio variations. Two-component fits show that most green galaxies have significant bulge and disc components and that the blue to red evolution is driven by colour change in the disc. Together, these strongly suggest that galaxies evolve from blue to red through secular disc fading and that a strong bulge is present prior to any decline in star formation. The relative abundance of the green population implies a typical time-scale for traversing the green valley ∼1–2 Gyr and is independent of environment, unlike that of the red and blue populations. While environment likely plays a rôle in triggering the passage across the green valley, it appears to have little effect on time taken. These results are consistent with a green valley population dominated by (early type) disc galaxies that are insufficiently supplied with gas to maintain previous levels of disc star formation, eventually attaining passive colours. No single event is needed to quench their star formation.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2018, the Author(s). This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1093/mnras/sty124en
dc.subjectGalaxies: bulgesen
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: star formationen
dc.subjectGalaxies: stellar contenten
dc.subjectGalaxies: structureen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleGalaxy and Mass Assembly (GAMA) : morphological transformation of galaxies across the green valleyen
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/sty124
dc.description.statusPeer revieweden


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