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dc.contributor.authorBoardman, N
dc.contributor.authorZasowski, G
dc.contributor.authorNewman, J A
dc.contributor.authorSanchez, S F
dc.contributor.authorAndrews, B
dc.contributor.authorBarrera-Ballesteros, J K
dc.contributor.authorLian, J
dc.contributor.authorRiffel, R
dc.contributor.authorRiffel, R A
dc.contributor.authorSchaefer, A
dc.contributor.authorBundy, K
dc.date.accessioned2022-06-07T14:30:15Z
dc.date.available2022-06-07T14:30:15Z
dc.date.issued2022-08
dc.identifier.citationBoardman , N , Zasowski , G , Newman , J A , Sanchez , S F , Andrews , B , Barrera-Ballesteros , J K , Lian , J , Riffel , R , Riffel , R A , Schaefer , A & Bundy , K 2022 , ' How well do local relations predict gas-phase metallicity gradients? Results from SDSS-IV MaNGA ' , Monthly Notices of the Royal Astronomical Society , vol. 514 , no. 2 , pp. 2298–2314 . https://doi.org/10.1093/mnras/stac1475en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 279835822
dc.identifier.otherPURE UUID: dfb4418f-0532-4598-b5f6-b7df672dd92b
dc.identifier.otherBibtex: 10.1093/mnras/stac1475
dc.identifier.otherWOS: 000811792300019
dc.identifier.urihttp://hdl.handle.net/10023/25503
dc.descriptionFunding: J.B-B thanks IA-100420 (DGAPA-PAPIIT, UNAM) and CONA-CYT grant CF19-39578 support. RR thanks Conselho Nacional de Desenvolvimento Científico e Tecnológico ( CNPq, Proj. 311223/2020-6, 304927/2017-1 and 400352/2016-8), Fundação de amparo ’a pesquisa do Rio Grande do Sul (FAPERGS, Proj. 16/2551-0000251-7 and 19/1750-2), Coordena¸cão de Aperfei¸coamento de Pessoal de Nível Superior (CAPES, Proj. 0001). RAR acknowledges financial support from Conselho Nacional de Desenvolvimento Científico e Tecnológico (302280/2019-7).en
dc.description.abstractGas-phase metallicity gradients in galaxies provide important clues to those galaxies’ formation histories. Using SDSS-IV MaNGA data, we previously demonstrated that gas metallicity gradients vary systematically and significantly across the galaxy mass–size plane: at stellar masses beyond approximately 1010 M⊙, more extended galaxies display steeper gradients (in units of dex/Re) at a given stellar mass. Here, we set out to develop a physical interpretation of these findings by examining the ability of local ∼kpc-scale relations to predict the gradient behaviour along the mass–size plane. We find that local stellar mass surface density, when combined with total stellar mass, is sufficient to reproduce the overall mass–size trend in a qualitative sense. We further find that we can improve the predictions by correcting for residual trends relating to the recent star formation histories of star-forming regions. However, we find as well that the most extended galaxies display steeper average gradients than predicted, even after correcting for residual metallicity trends with other local parameters. From these results, we argue that gas-phase metallicity gradients can largely be understood in terms of known local relations, but we also discuss some possible physical causes of discrepant gradients.
dc.format.extent21
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2022 The Author(s) Published by Oxford University Press on behalf of 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/stac1475.en
dc.subjectGalaxies: ISMen
dc.subjectGalaxies: structureen
dc.subjectGalaxies: generalen
dc.subjectGalaxies: statisticsen
dc.subjectISM: abundancesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleHow well do local relations predict gas-phase metallicity gradients? Results from SDSS-IV MaNGAen
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/stac1475
dc.description.statusPeer revieweden


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