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dc.contributor.authorVulcani, Benedetta
dc.contributor.authorBamford, Steven P.
dc.contributor.authorHaeussler, Boris
dc.contributor.authorVika, Marina
dc.contributor.authorRojas, Alex
dc.contributor.authorAgius, Nicola K.
dc.contributor.authorBaldry, Ivan
dc.contributor.authorBauer, Amanda E.
dc.contributor.authorBrown, Michael J. I.
dc.contributor.authorDriver, Simon
dc.contributor.authorGraham, Alister W.
dc.contributor.authorKelvin, Lee S.
dc.contributor.authorLiske, Jochen
dc.contributor.authorLoveday, Jon
dc.contributor.authorPopescu, Cristina C.
dc.contributor.authorRobotham, Aaron S. G.
dc.contributor.authorTuffs, Richard J.
dc.date.accessioned2014-07-24T09:31:05Z
dc.date.available2014-07-24T09:31:05Z
dc.date.issued2014-06
dc.identifier.citationVulcani , B , Bamford , S P , Haeussler , B , Vika , M , Rojas , A , Agius , N K , Baldry , I , Bauer , A E , Brown , M J I , Driver , S , Graham , A W , Kelvin , L S , Liske , J , Loveday , J , Popescu , C C , Robotham , A S G & Tuffs , R J 2014 , ' Galaxy And Mass Assembly (GAMA) : the wavelength-dependent sizes and profiles of galaxies revealed by MegaMorph ' , Monthly Notices of the Royal Astronomical Society , vol. 441 , no. 2 , pp. 1340-1362 . https://doi.org/10.1093/mnras/stu632en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 134747879
dc.identifier.otherPURE UUID: 6f2d57d8-40a4-40f4-b129-8f01b61a615f
dc.identifier.otherWOS: 000336494800034
dc.identifier.otherScopus: 84900560050
dc.identifier.otherWOS: 000336494800034
dc.identifier.urihttp://hdl.handle.net/10023/5069
dc.description.abstractWe investigate the relationship between colour and structure within galaxies using a large, volume-limited sample of bright, low-redshift galaxies with optical-near-infrared imaging from the Galaxy And Mass Assembly survey. We fit single-component, wavelength-dependent, elliptical S,rsic models to all passbands simultaneously, using software developed by the MegaMorph project. Dividing our sample by n and colour, the recovered wavelength variations in effective radius (R-e) and S,rsic index (n) reveal the internal structure, and hence formation history, of different types of galaxies. All these trends depend on n; some have an additional dependence on galaxy colour. Late-type galaxies (n(r) <2.5) show a dramatic increase in S,rsic index with wavelength. This might be a result of their two-component (bulge-disc) nature, though stellar population gradients within each component and dust attenuation are likely to play a role. All galaxies show a substantial decrease in R-e with wavelength. This is strongest for early types (n(r) > 2.5), even though they maintain constant n with wavelength, revealing that ellipticals are a superimposition of different stellar populations associated with multiple collapse and merging events. Processes leading to structures with larger R-e must be associated with lower metallicity or younger stellar populations. This appears to rule out the formation of young cores through dissipative gas accretion as an important mechanism in the recent lives of luminous elliptical galaxies.
dc.format.extent23
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2014. The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.en
dc.subjectGalaxies: formationen
dc.subjectGalaxies: fundamental parametersen
dc.subjectGalaxies: generalen
dc.subjectGalaxies: structureen
dc.subjectDisk-dominated galaxiesen
dc.subjectDigital sky surveyen
dc.subjectStellar population gradientsen
dc.subjectBand surface photometryen
dc.subjectRadial color gradientsen
dc.subjectElliptic galaxiesen
dc.subjectSpiral galaxiesen
dc.subjectCluster galaxiesen
dc.subjectPhysical-propertiesen
dc.subjectFundamental planeen
dc.subjectQB Astronomyen
dc.subject.lccQBen
dc.titleGalaxy And Mass Assembly (GAMA) : the wavelength-dependent sizes and profiles of galaxies revealed by MegaMorphen
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/stu632
dc.description.statusPeer revieweden


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