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dc.contributor.authorVincenzo, Fiorenzo
dc.contributor.authorKobayashi, Chiaki
dc.contributor.authorTaylor, Philip
dc.date.accessioned2018-08-16T00:18:12Z
dc.date.available2018-08-16T00:18:12Z
dc.date.issued2018-10-01
dc.identifier.citationVincenzo , F , Kobayashi , C & Taylor , P 2018 , ' On the [α/Fe]-[Fe/H] relations in early-type galaxies ' , Monthly Notices of the Royal Astronomical Society: Letters , vol. 480 , no. 1 , pp. L38–L42 . https://doi.org/10.1093/mnrasl/sly128
dc.identifier.issn1745-3925
dc.identifier.otherPURE: 15022253
dc.identifier.otherPURE UUID: 826699fb-a67a-400d-b38f-1d916a9e8fcb
dc.identifier.otherScopus: 85054761727
dc.identifier.otherORCID: /0000-0002-4343-0487/work/62750495
dc.identifier.urihttp://hdl.handle.net/2299/20461
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
dc.description.abstractWe study how the predicted [α/Fe]-[Fe/H] relations in early-type galaxies vary as functions of their stellar masses, ages, and stellar velocity dispersions, by making use of cosmological chemodynamical simulations with feedback from active galactic nuclei. Our model includes a detailed treatment for the chemical enrichment from dying stars, core-collapse supernovae (both Type II and hypernovae) and Type Ia supernovae. At redshift z = 0, we create a catalogue of 526 galaxies, among which we determine 80 early-type galaxies. From the analysis of our simulations, we find [α/Fe]-[Fe/H] relations similar to the Galactic bulge. We also find that, in the oldest galaxies, Type Ia supernovae start to contribute at higher [Fe/H] than in the youngest ones. On the average, early-type galaxies with larger stellar masses (and, equivalently, higher stellar velocity dispersions) have higher [α/Fe] ratios, at fixed [Fe/H]. This is qualitatively consistent with the recent observations of Sybilska et al., but quantitatively there are mismatches, which might require stronger feedback, sub-classes of Type Ia Supernovae, or a variable initial mass function to address.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society: Letters
dc.rightsOpen
dc.subjectCD- galaxies: evolution
dc.subjectGalaxies: abundances
dc.subjectGalaxies: elliptical and lenticular
dc.subjectHydrodynamics
dc.subjectStars: abundances
dc.subjectSupernovae: general
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleOn the [α/Fe]-[Fe/H] relations in early-type galaxiesen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85054761727&partnerID=8YFLogxK
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2018-10-01
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnrasl/sly128
rioxxterms.licenseref.uriOther
rioxxterms.typeOther
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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