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dc.contributor.authorCashmore, CRen
dc.contributor.authorWilkinson, MIen
dc.contributor.authorPower, Cen
dc.contributor.authorBourne, Martinen
dc.date.accessioned2017-06-12T08:53:57Z
dc.date.available2017-06-12T08:53:57Z
dc.date.issued2017-06-01en
dc.identifier.issn0035-8711
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/264709
dc.description.abstractWe present high-resolution simulations of an isolated dwarf spheroidal (dSph) galaxy between redshifts z ∼ 10 and z ∼ 4, the epoch when several Milky Way dSph satellites experienced extended star formation, in order to understand in detail the physical processes which affect a low-mass halo's ability to retain gas. It is well established that supernova feedback is very effective at expelling gas from a 3 × 10$^{7}$ M⊙ halo, the mass of a typical redshift 10 progenitor of a redshift 0 halo with mass ∼10$^{9}$ M⊙. We investigate the conditions under which such a halo is able to retain sufficient high-density gas to support extended star formation. In particular, we explore the effects of: an increased relative concentration of the gas compared to the dark matter; a higher concentration dark matter halo; significantly lower supernova rates; enhanced metal cooling due to enrichment from earlier supernovae. We show that disc-like gas distributions retain more gas than spherical ones, primarily due to the shorter gas cooling times in the disc. However, a significant reduction in the number of supernovae compared to that expected for a standard initial mass function is still needed to allow the retention of high-density gas. We conclude that the progenitors of the observed dSphs would only have retained the gas required to sustain star formation if their mass, concentration and gas morphology were already unusual for those of a dSph-mass halo progenitor by a redshift of 10.
dc.description.sponsorshipCRC and MAB are supported by a Science and Technology facilities council (STFC) PhD studentship. CP acknowledges support from the Australian Research Council (ARC) Future Fellowship FT130100041 and Discovery projects DP130100117 and DP140100198. Figs 4 and 6 were produced using SPLASH (Price 2013). This work used the DiRAC Complexity system, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment is funded by BIS National E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations grant ST/K0003259/1. DiRAC is part of the National E-Infrastructure.
dc.languageengen
dc.language.isoenen
dc.publisherOxford University Press
dc.subjectsupernovae: individualen
dc.subjectgalaxies: dwarfen
dc.subjectgalaxies: evolutionen
dc.subjectgalaxies: formationen
dc.subjectgalaxies: ISMen
dc.titleToo small to succeed: the difficulty of sustaining star formation in low-mass haloesen
dc.typeArticle
prism.endingPage468
prism.issueIdentifier1en
prism.publicationDate2017en
prism.publicationNameMonthly Notices of the Royal Astronomical Societyen
prism.startingPage451
prism.volume468en
dc.identifier.doi10.17863/CAM.10376
dcterms.dateAccepted2017-02-01en
rioxxterms.versionofrecord10.1093/mnras/stx315en
rioxxterms.versionVoRen
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserveden
rioxxterms.licenseref.startdate2017-06-01en
dc.contributor.orcidBourne, Martin [0000-0003-3189-1638]
dc.identifier.eissn1365-2966
rioxxterms.typeJournal Article/Reviewen
pubs.funder-project-idECH2020 EUROPEAN RESEARCH COUNCIL (ERC) (638707)
cam.issuedOnline2017-02-08en
cam.orpheus.successThu Jan 30 12:53:49 GMT 2020 - The item has an open VoR version.*
rioxxterms.freetoread.startdate2100-01-01


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