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dc.contributor.authorVincenzo, Fiorenzo
dc.contributor.authorMatteucci, Francesca
dc.contributor.authorRecchi, Simone
dc.contributor.authorCalura, Francesco
dc.contributor.authorMcWilliam, Andrew
dc.contributor.authorLanfranchi, Gustavo A.
dc.date.accessioned2017-08-11T15:06:29Z
dc.date.available2017-08-11T15:06:29Z
dc.date.issued2015-05-11
dc.identifier.citationVincenzo , F , Matteucci , F , Recchi , S , Calura , F , McWilliam , A & Lanfranchi , G A 2015 , ' The IGIMF and other IMFs in dSphs: the case of Sagittarius ' , Monthly Notices of the Royal Astronomical Society , vol. 449 , no. 2 , stv357 , pp. 1327-1339 . https://doi.org/10.1093/mnras/stv357
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 11927566
dc.identifier.otherPURE UUID: bff38b41-876a-4615-8bfd-4d8bf13fd2a4
dc.identifier.otherArXiv: http://arxiv.org/abs/1502.05221v3
dc.identifier.otherScopus: 84983068765
dc.identifier.urihttp://hdl.handle.net/2299/19223
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved
dc.description.abstractWe have studied the effects of various initial mass functions (IMFs) on the chemical evolution of the Sagittarius dwarf galaxy (Sgr). In particular, we tested the effects of the integrated galactic initial mass function (IGIMF) on various predicted abundance patterns. The IGIMF depends on the star formation rate and metallicity and predicts less massive stars in a regime of low star formation, as it is the case in dwarf spheroidals. We adopted a detailed chemical evolution model following the evolution of α-elements, Fe and Eu, and assuming the currently best set of stellar yields. We also explored different yield prescriptions for the Eu, including production from neutron star mergers. Although the uncertainties still present in the stellar yields and data prevent us from drawing firm conclusions, our results suggest that the IGIMF applied to Sgr predicts lower [α/Fe] ratios than classical IMFs and lower [hydrostatic/explosive] α-element ratios, in qualitative agreement with observations. In our model, the observed high [Eu/O] ratios in Sgr is due to reduced O production, resulting from the IGIMF mass cut-off of the massive oxygen-producing stars, as well as to the Eu yield produced in neutron star mergers, a more promising site than core-collapse supernovae, although many uncertainties are still present in the Eu nucleosynthesis. We find that a model, similar to our previous calculations, based on the late addition of iron from the Type Ia supernova time-delay (necessary to reproduce the shape of [X/Fe] versus [Fe/H] relations) but also including the reduction of massive stars due to the IGIMF, better reproduces the observed abundance ratios in Sgr than models without the IGIMF.en
dc.format.extent13
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.subjectstars: abundances
dc.subjectgalaxies: abundances
dc.subjectgalaxies: dwarf
dc.subjectgalaxies: evolution
dc.subjectgalaxies: formation
dc.subjectLocal Group
dc.titleThe IGIMF and other IMFs in dSphs: : the case of Sagittariusen
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.dateAccepted2015-02-18
rioxxterms.versionAM
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stv357
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeopenAccess


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