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dc.contributor.authorLegrand, Laurent
dc.contributor.authorHutter, Anne
dc.contributor.authorDayal, Pratika
dc.contributor.authorUcci, Graziano
dc.contributor.authorGottlöber, Stefan
dc.contributor.authorYepes Alonso, Gustavo 
dc.contributor.otherUAM. Departamento de Física Teóricaes_ES
dc.date.accessioned2022-09-26T12:02:10Z
dc.date.available2022-09-26T12:02:10Z
dc.date.issued2021-10-25
dc.identifier.citationMonthly Notices of the Royal Astronomical Society 509.1 (2022): 595-613es_ES
dc.identifier.issn0035-8711 (print)es_ES
dc.identifier.issn1365-2966 (online)es_ES
dc.identifier.urihttp://hdl.handle.net/10486/704276
dc.descriptionThis is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Monthly Notices of the Royal Astronomical Society 509.1 (2022): 595-613 is available online at: https://academic.oup.com/mnras/article-abstract/509/1/595/6409841?redirectedFrom=fulltext#no-access-messagees_ES
dc.description.abstractWe use the astraeus framework, that couples an N-body simulation with a semi-analytic model for galaxy formation and a semi-numerical model for reionization, to quantify the star formation histories (SFHs) of galaxies in the first billion years. Exploring four models of radiative feedback, we fit the SFH of each galaxy at 𝑧 > 5 as log(SFR(𝑧)) = −𝛼(1 + 𝑧) + 𝛽; star formation is deemed stochastic if it deviates from this fit by more than ΔSFR = 0.6 dex. Our key findings are: (i) The fraction of stellar mass formed and time spent in the stochastic phase decrease with increasing stellar mass and redshift 𝑧. While galaxies with stellar masses of 𝑀★ ∼ 107M at 𝑧 ∼ 5 (10) form ∼ 70% (20%) of their stellar mass in the stochastic phase, this reduces to < 10% at all redshifts for galaxies with 𝑀★ > 1010M ; (ii) the fractional mass assembled and lifetime spent in the stochastic phase do not significantly change with the radiative feedback model used; (iii) at all redshifts, 𝛼 increases (decreases for the strongest radiative feedback model) with stellar mass for galaxies with 𝑀★ <∼ 108.5M and converges to ∼ 0.18 for more massive galaxies; 𝛽 always increases with stellar mass. Our proposed fits can reliably recover the stellar masses and mass-to-light ratios for galaxies with 𝑀★ ∼ 108−10.5M and MUV ∼ −17 to − 23 at 𝑧 ∼ 5 − 9. This physical model can therefore be used to derive the SFHs for galaxies observed by a number of forthcoming instrumentses_ES
dc.format.extent20 pag.es_ES
dc.format.mimetypeapplication/pdfes_ES
dc.language.isoenges_ES
dc.publisherRoyal Astronomical Societyes_ES
dc.publisherOxford University Presses_ES
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyes_ES
dc.rights© 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Societyes_ES
dc.subject.otherMethods: Numericales_ES
dc.subject.otherGalaxy: Evolutiones_ES
dc.subject.otherGalaxies: High-Redshiftes_ES
dc.subject.otherGalaxies: Star Formationes_ES
dc.subject.otherGalaxies: Stellar Contentes_ES
dc.subject.otherDark Ages, Reionizationes_ES
dc.subject.otherFirst Starses_ES
dc.titleAstraeus IV: Quantifying the star foation histories of galaxies in the Epoch of Reionizationes_ES
dc.typearticlees_ES
dc.subject.ecienciaFísicaes_ES
dc.relation.publisherversionhttps://doi.org/10.1093/mnras/stab3034es_ES
dc.identifier.doi10.1093/mnras/stab3034es_ES
dc.identifier.publicationfirstpage595es_ES
dc.identifier.publicationissue1es_ES
dc.identifier.publicationlastpage613es_ES
dc.identifier.publicationvolume509es_ES
dc.relation.projectIDinfo:eu-repo/grantAgreement/EC/H2020/717001/EU//DELPHIes_ES
dc.relation.projectIDGobierno de España. AYA2015-63810-Pes_ES
dc.relation.projectIDGobierno de España. PGC2018-094975-C21es_ES
dc.type.versioninfo:eu-repo/semantics/acceptedVersiones_ES
dc.rights.accessRightsopenAccesses_ES
dc.facultadUAMFacultad de Cienciases_ES
dc.institutoUAMCentro de Investigación Avanzada en Física Fundamental (CIAFF)es_ES


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