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dc.contributor.authorVincenzo, Fiorenzo
dc.contributor.authorBelfiore, Francesco
dc.contributor.authorMaiolino, Roberto
dc.contributor.authorMatteucci, Francesca
dc.contributor.authorVentura, Paolo
dc.date.accessioned2017-08-08T12:59:27Z
dc.date.available2017-08-08T12:59:27Z
dc.date.issued2016-06-01
dc.identifier.citationVincenzo , F , Belfiore , F , Maiolino , R , Matteucci , F & Ventura , P 2016 , ' Nitrogen and oxygen abundances in the Local Universe ' , Monthly Notices of the Royal Astronomical Society , vol. 458 , no. 4 , stw532 , pp. 3466-3477 . https://doi.org/10.1093/mnras/stw532
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 11927505
dc.identifier.otherPURE UUID: acdd63db-7702-4e19-b6a9-6fd4272819e1
dc.identifier.otherArXiv: http://arxiv.org/abs/1603.00460v1
dc.identifier.otherScopus: 84965017976
dc.identifier.urihttp://hdl.handle.net/2299/19181
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. ©: 2016 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
dc.description.abstractWe present chemical evolution models aimed at reproducing the observed (N/O) versus (O/H) abundance pattern of star-forming galaxies in the Local Universe. We derive gas-phase abundances from Sloan Digital Sky Survey (SDSS) spectroscopy and a complementary sample of low-metallicity dwarf galaxies, making use of a consistent set of abundance calibrations. This collection of data clearly confirms the existence of a plateau in the (N/O) ratio at very low metallicity, followed by an increase of this ratio up to high values as the metallicity increases. This trend can be interpreted as due to two main sources of nitrogen in galaxies: (i) massive stars, which produce small amounts of pure primary nitrogen and are responsible for the (N/O) ratio in the low-metallicity plateau; (ii) low- and intermediate-mass stars, which produce both secondary and primary nitrogen and enrich the interstellar medium with a time delay relative to massive stars, and cause the increase of the (N/O) ratio. We find that the length of the low-metallicity plateau is almost solely determined by the star formation efficiency, which regulates the rate of oxygen production by massive stars. We show that, to reproduce the high observed (N/O) ratios at high (O/H), as well as the right slope of the (N/O) versus (O/H) curve, a differential galactic wind – where oxygen is assumed to be lost more easily than nitrogen – is necessary. No existing set of stellar yields can reproduce the observed trend without assuming differential galactic winds. Finally, considering the current best set of stellar yields, a bottom-heavy initial mass function is favoured to reproduce the data.en
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.subjectstars: abundances
dc.subjectISM: abundances
dc.subjectISM: evolution
dc.subjectgalaxies: abundances
dc.subjectgalaxies: evolution
dc.subjectgalaxies: ISM
dc.titleNitrogen and oxygen abundances in the Local Universeen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2016-03-02
rioxxterms.versionAM
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stw532
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeopenAccess


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