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dc.contributor.authorVincenzo, Fiorenzo
dc.contributor.authorMatteucci, Francesca
dc.contributor.authorDe Boer, Thomas J L
dc.contributor.authorCignoni, Michele
dc.contributor.authorTosi, Monica
dc.date.accessioned2017-08-07T15:27:49Z
dc.date.available2017-08-07T15:27:49Z
dc.date.issued2016-08-01
dc.identifier.citationVincenzo , F , Matteucci , F , De Boer , T J L , Cignoni , M & Tosi , M 2016 , ' Lighting up stars in chemical evolution models : the CMD of Sculptor ' , Monthly Notices of the Royal Astronomical Society , vol. 460 , no. 2 , pp. 2238-2244 . https://doi.org/10.1093/mnras/stw1145
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 11927528
dc.identifier.otherPURE UUID: 9feef8b8-6966-40b8-8dd7-b6d885d78422
dc.identifier.otherArXiv: http://arxiv.org/abs/1605.03606v1
dc.identifier.otherScopus: 84983049818
dc.identifier.urihttp://hdl.handle.net/2299/19165
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 a novel approach to draw the synthetic colour–magnitude diagram (CMD) of galaxies, which can provide – in principle – a deeper insight in the interpretation and understanding of current observations. In particular, we ‘light up’ the stars of chemical evolution models, according to their initial mass, metallicity and age, to eventually understand how the assumed underlying galaxy formation and evolution scenario affects the final configuration of the synthetic CMD. In this way, we obtain a new set of observational constraints for chemical evolution models beyond the usual photospheric chemical abundances. The strength of our method resides in the very fine grid of metallicities and ages of the assumed data base of stellar isochrones. In this work, we apply our photochemical model to reproduce the observed CMD of the Sculptor dSph and find that we can reproduce the main features of the observed CMD. The main discrepancies are found at fainter magnitudes in the main sequence turn-off and sub-giant branch, where the observed CMD extends towards bluer colours than the synthetic one; we suggest that this is a signature of metal-poor stellar populations in the data, which cannot be captured by our assumed one-zone chemical evolution model.en
dc.format.extent7
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectstars: abundances
dc.subjectHertzprung-Russell and colour-magniture diagrams
dc.subjectdwarf
dc.subjectLocal Group
dc.subjectgalaxies: stellar content
dc.titleLighting up stars in chemical evolution models : the CMD of Sculptoren
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stw1145
rioxxterms.typeJournal Article/Review


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