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dc.contributor.authorDe Propris, Roberto
dc.contributor.authorBaldry, Ivan K.
dc.contributor.authorBland-Hawthorn, Joss
dc.contributor.authorBrough, Sarah
dc.contributor.authorDriver, Simon P.
dc.contributor.authorHopkins, Andrew M.
dc.contributor.authorKelvin, Lee
dc.contributor.authorLoveday, Jon
dc.contributor.authorPhillipps, Steve
dc.contributor.authorRobotham, Aaron S. G.
dc.date.accessioned2014-11-21T17:31:02Z
dc.date.available2014-11-21T17:31:02Z
dc.date.issued2014-11-01
dc.identifier.citationDe Propris , R , Baldry , I K , Bland-Hawthorn , J , Brough , S , Driver , S P , Hopkins , A M , Kelvin , L , Loveday , J , Phillipps , S & Robotham , A S G 2014 , ' Galaxy and Mass Assembly (GAMA) : merging galaxies and their properties ' , Monthly Notices of the Royal Astronomical Society , vol. 444 , no. 3 , pp. 2200-2211 . https://doi.org/10.1093/mnras/stu1452en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 157934258
dc.identifier.otherPURE UUID: bcd5d5a6-48a2-44c3-a90c-686fe92a14ba
dc.identifier.otherWOS: 000343399600019
dc.identifier.otherScopus: 84908420634
dc.identifier.otherWOS: 000343399600019
dc.identifier.urihttp://hdl.handle.net/10023/5830
dc.description.abstractWe derive the close pair fractions and volume merger rates for galaxies in the Galaxy and Mass Assembly (GAMA) survey with -23 <M-r <-17 (Omega(M) = 0.27, Omega(A) = 0.73, H-0 = 100 km s(-1) Mpc(-1)) at 0.01 <z <0.22 (look-back time of <2 Gyr). The merger fraction is approximately 1.5 per cent Gyr(-1) at all luminosities (assuming 50 per cent of pairs merge) and the volume merger rate is approximate to 3.5 x 10(-4) Mpc(-3) Gyr(-1). We examine how the merger rate varies by luminosity and morphology. Dry mergers (between red/spheroidal galaxies) are found to be uncommon and to decrease with decreasing luminosity. Fainter mergers are wet, between blue/discy galaxies. Damp mergers (one of each type) follow the average of dry and wetmergers. In the brighter luminosity bin (-23 <M-r <-20), the merger rate evolution is flat, irrespective of colour or morphology, out to z similar to 0.2. The makeup of the merging population does not appear to change over this redshift range. Galaxy growth by major mergers appears comparatively unimportant and dry mergers are unlikely to be significant in the buildup of the red sequence over the past 2 Gyr. We compare the colour, morphology, environmental density and degree of activity (BPT class, Baldwin, Phillips & Terlevich) of galaxies in pairs to those of more isolated objects in the same volume. Galaxies in close pairs tend to be both redder and slightly more spheroid dominated than the comparison sample. We suggest that this may be due to 'harassment' in multiple previous passes prior to the current close interaction. Galaxy pairs do not appear to prefer significantly denser environments. There is no evidence of an enhancement in the AGN fraction in pairs, compared to other galaxies in the same volume.
dc.format.extent12
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. This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society All rights reserved.en
dc.subjectgalaxies: formationen
dc.subjectgalaxies: interactionsen
dc.subjectDigital sky surveyen
dc.subjectSimilar-to 1en
dc.subjectSupermassive black-holesen
dc.subjectStar-forming galaxiesen
dc.subjectLuminous red galaxiesen
dc.subjectMerger rate evolutionen
dc.subjectCold dark-matteren
dc.subjectLess-than 1.5en
dc.subjectRedshift surveyen
dc.subjectElliptic galaxiesen
dc.subjectQC Physicsen
dc.subjectQB Astronomyen
dc.subject.lccQCen
dc.subject.lccQBen
dc.titleGalaxy and Mass Assembly (GAMA) : merging galaxies and their propertiesen
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/stu1452
dc.description.statusPeer revieweden


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