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dc.contributor.authorRiaz, B.
dc.contributor.authorLodieu, N.
dc.contributor.authorGoodwin, S.
dc.contributor.authorStamatellos, D.
dc.contributor.authorThompson, M.
dc.date.accessioned2012-03-05T14:00:51Z
dc.date.available2012-03-05T14:00:51Z
dc.date.issued2012-03-01
dc.identifier.citationRiaz , B , Lodieu , N , Goodwin , S , Stamatellos , D & Thompson , M 2012 , ' Disc frequencies for brown dwarfs in the Upper Scorpius OB association : implications for brown dwarf formation theories ' , Monthly Notices of the Royal Astronomical Society , vol. 420 , no. 3 , pp. 2497-2517 . https://doi.org/10.1111/j.1365-2966.2011.20214.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 625357
dc.identifier.otherPURE UUID: 21bd4e1e-84ce-4ffe-8ba3-3b50cf2ba2fe
dc.identifier.otherBibtex: urn:c3f63b763d2917798fe39a3c84392c7a
dc.identifier.otherScopus: 84857036507
dc.identifier.urihttp://hdl.handle.net/2299/7900
dc.description.abstractWe have investigated the brown dwarf (BD) and stellar disc fractions in the Upper Scorpius OB Association (USco) and compared them with several other young regions. We have compiled the most complete sample of of all spectroscopically confirmed BDs in USco, and have made use of the WISE catalog to identify the disc candidates. We report on the discovery of 12 new BD discs in USco, with spectral type (SpT) between M6 and M8.5. The WISE colors for the new discs are similar to the primordial (transition) discs earlier detected in USco. Combining with previous surveys, we find the lowest inner disc fractions (~20-25%) for a wide range in stellar masses (~0.01-4.0 Msun) in the USco association. The low disc fractions for high-mass stars in USco (and the other clusters) are consistent with an evolutionary decline in inner disc frequency with age. However, BD disc fractions are higher than those for the stars in 1-3 Myr clusters, but very low in the ~5 Myr old USco. Also, primordial BD discs are still visible in the ~10 Myr TW Hydrae association, whereas the higher mass stars have all transitioned to the debris stage by this age. The disc frequencies for BDs do not show any dependence on the stellar density or the BD/star number ratio in a cluster. We suggest that the large differences in the observed BD disc fractions between regions may well be due to different BD formation mechanisms and therefore different initial disc fractions/properties. We also present a WISE SED classification scheme, based on the Ks and WISE bands of 3.4-12micron, to distinguish between the Class I/II and the Class III sequence. Our work includes a comparison of the sensitivities of WISE and Spitzer disc surveys. We estimate that WISE can be incomplete for discs at SpT later than M8 in distant clusters such as SOri. WISE should be able to recover the M8-M9 discs in the nearby young clustersen
dc.format.extent21
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.subjectstars: low-mass, open clusters and associations: individual: Upper Scorpius OB association
dc.subjectbrown dwarfs
dc.subjectcircumstellar matter
dc.titleDisc frequencies for brown dwarfs in the Upper Scorpius OB association : implications for brown dwarf formation theoriesen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
dcterms.dateAccepted2012-03-01
rioxxterms.versionVoR
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2011.20214.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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