dc.contributor.author Taylor, Philip dc.contributor.author Federrath, Christoph dc.contributor.author Kobayashi, Chiaki dc.date.accessioned 2018-09-12T15:20:58Z dc.date.available 2018-09-12T15:20:58Z dc.date.issued 2017-08-21 dc.identifier.citation Taylor , P , Federrath , C & Kobayashi , C 2017 , ' Star formation in simulated galaxies: understanding the transition to quiescence at 3 × 1010 M⊙ ' Monthly Notices of the Royal Astronomical Society , vol. 469 , no. 4 , pp. 4249–4257 . https://doi.org/10.1093/mnras/stx1128 dc.identifier.issn 0035-8711 dc.identifier.other PURE: 14856567 dc.identifier.other PURE UUID: 6e23e4d1-4bdd-4c6f-8294-7523c31a6bc4 dc.identifier.other ArXiv: http://arxiv.org/abs/1705.03173v1 dc.identifier.uri https://arxiv.org/abs/1705.03173 dc.description This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. © 2017 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. dc.description.abstract Star formation in galaxies relies on the availability of cold, dense gas, which, in turn, relies on factors internal and external to the galaxies. In order to provide a simple model for how star formation is regulated by various physical processes in galaxies, we analyse data at redshift $z=0$ from a hydrodynamical cosmological simulation that includes prescriptions for star formation and stellar evolution, active galactic nuclei (AGN), and their associated feedback processes. This model can determine the star formation rate (SFR) as a function of galaxy stellar mass, gas mass, black hole mass, and environment. We find that gas mass is the most important quantity controlling star formation in low-mass galaxies, and star-forming galaxies in dense environments have higher SFR than their counterparts in the field. In high-mass galaxies, we find that black holes more massive than $\sim10^{7.5}$ M$_\odot$ can be triggered to quench star formation in their host; this mass scale is emergent in our simulations. Furthermore, this black hole mass corresponds to a galaxy bulge mass $\sim2\times10^{10}$ M$_\odot$, consistent with the mass at which galaxies start to become dominated by early types ($\sim3\times10^{10}$ M$_\odot$, as previously shown in observations by Kauffmann et al.). Finally, we demonstrate that our model can reproduce well the SFR measured from observations of galaxies in the GAMA and ALFALFA surveys. en dc.language.iso eng dc.relation.ispartof Monthly Notices of the Royal Astronomical Society dc.rights /dk/atira/pure/core/openaccesspermission/open dc.subject astro-ph.GA dc.title Star formation in simulated galaxies: understanding the transition to quiescence at 3 × 1010 M⊙ en dc.contributor.institution Centre for Astrophysics Research dc.contributor.institution School of Physics, Astronomy and Mathematics dc.description.status Peer reviewed dc.identifier.url https://arxiv.org/abs/1705.03173 dc.relation.school School of Physics, Astronomy and Mathematics dc.description.versiontype Final Accepted Version dcterms.dateAccepted 2017-05-07 rioxxterms.version AM rioxxterms.versionofrecord https://doi.org/10.1093/mnras/stx1128 rioxxterms.type Journal Article/Review herts.preservation.rarelyaccessed true herts.rights.accesstype openAccess
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