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dc.contributor.authorBellstedt, Sabine
dc.contributor.authorRobotham, Aaron S. G.
dc.contributor.authorDriver, Simon P.
dc.contributor.authorThorne, Jessica E.
dc.contributor.authorDavies, Luke J. M.
dc.contributor.authorLagos, Claudia del P.
dc.contributor.authorStevens, Adam R. H.
dc.contributor.authorTaylor, Edward N.
dc.contributor.authorBaldry, Ivan K.
dc.contributor.authorMoffett, Amanda J.
dc.contributor.authorHopkins, Andrew M.
dc.contributor.authorPhillipps, Steven
dc.date.accessioned2020-12-07T15:59:16Z
dc.date.available2020-12-07T15:59:16Z
dc.date.issued2020-11
dc.identifier.citationBellstedt , S , Robotham , A S G , Driver , S P , Thorne , J E , Davies , L J M , Lagos , C D P , Stevens , A R H , Taylor , E N , Baldry , I K , Moffett , A J , Hopkins , A M & Phillipps , S 2020 , ' Galaxy And Mass Assembly (GAMA) : a forensic SED reconstruction of the cosmic star formation history and metallicity evolution by galaxy type ' , Monthly Notices of the Royal Astronomical Society , vol. 498 , no. 4 , pp. 5581-5603 . https://doi.org/10.1093/mnras/staa2620en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 271521355
dc.identifier.otherPURE UUID: c2816ef1-0282-41c3-b10c-3e519b835171
dc.identifier.otherWOS: 000587755500073
dc.identifier.otherScopus: 85095849904
dc.identifier.urihttp://hdl.handle.net/10023/21113
dc.descriptionSB and SPD acknowledge support by the Australian Research Council’s funding scheme DP180103740.en
dc.description.abstractWe apply the spectral energy distribution (SED) fitting code PROSPECT to multiwavelength imaging for similar to 7000 galaxies from the GAMA survey at z <0.06, in order to extract their star formation histories. We combine a parametric description of the star formation history with a closed-box evolution of metallicity where the present-day gas-phase metallicity of the galaxy is a free parameter. We show with this approach that we are able to recover the observationally determined cosmic star formation history (CSFH), an indication that stars are being formed in the correct epoch of the Universe, on average, for the manner in which we are conducting SED fitting. We also show the contribution to the CSFH of galaxies of different present-day visual morphologies and stellar masses. Our analysis suggests that half of the mass in present-day elliptical galaxies was in place 11 Gyr ago. In other morphological types, the stellar mass formed later, up to 6 Gyr ago for present-day irregular galaxies. Similarly, the most massive galaxies in our sample were shown to have formed half their stellar mass by 11 Gyr ago, whereas the least massive galaxies reached this stage as late as 4 Gyr ago (the well-known effect of 'galaxy downsizing'). Finally, our metallicity approach allows us to follow the average evolution in gas-phase metallicity for populations of galaxies and extract the evolution of the cosmic metal mass density in stars and in gas, producing results in broad agreement with independent, higher redshift observations of metal densities in the Universe.
dc.format.extent23
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2020 the Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/staa2620.en
dc.subjectGalaxies: elliptical and lenticular, cDen
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: generalen
dc.subjectGalaxies: photometryen
dc.subjectGalaxies: spiralen
dc.subjectGalaxies: star formationen
dc.subjectQC Physicsen
dc.subjectQB Astronomyen
dc.subjectDASen
dc.subject.lccQCen
dc.subject.lccQBen
dc.titleGalaxy And Mass Assembly (GAMA) : a forensic SED reconstruction of the cosmic star formation history and metallicity evolution by galaxy typeen
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/staa2620
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/2005.11917en


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