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dc.contributor.authorSmart, R. L.
dc.contributor.authorMarocco, F.
dc.contributor.authorSarro, L. M.
dc.contributor.authorBarrado, D.
dc.contributor.authorBeamin, J. C.
dc.contributor.authorCaballero, J. A.
dc.contributor.authorJones, H. R. A.
dc.date.accessioned2019-07-29T11:19:16Z
dc.date.available2019-07-29T11:19:16Z
dc.date.issued2019-05-01
dc.identifier.citationSmart , R L , Marocco , F , Sarro , L M , Barrado , D , Beamin , J C , Caballero , J A & Jones , H R A 2019 , ' The Gaia Ultra-Cool Dwarf Sample -- II : Structure at the end of the main sequence ' , Monthly Notices of the Royal Astronomical Society , vol. 485 , no. 3 , pp. 4423–4440 . https://doi.org/10.1093/mnras/stz678
dc.identifier.issn0035-8711
dc.identifier.otherArXiv: http://arxiv.org/abs/1902.07571v1
dc.identifier.urihttp://hdl.handle.net/2299/21484
dc.description© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
dc.description.abstractWe identify and investigate known late M, L, and T dwarfs in the Gaia second data release. This sample is being used as a training set in the Gaia data processing chain of the ultracool dwarfs work package. We find 695 objects in the optical spectral range M8–T6 with accurate Gaia coordinates, proper motions, and parallaxes which we combine with published spectral types and photometry from large area optical and infrared sky surveys. We find that 100 objects are in 47 multiple systems, of which 27 systems are published and 20 are new. These will be useful benchmark systems and we discuss the requirements to produce a complete catalogue of multiple systems with an ultracool dwarf component. We examine the magnitudes in the Gaia passbands and find that the G BP magnitudes are unreliable and should not be used for these objects. We examine progressively redder colour–magnitude diagrams and see a notable increase in the main-sequence scatter and a bivariate main sequence for old and young objects. We provide an absolute magnitude – spectral subtype calibration for G and G RP passbands along with linear fits over the range M8–L8 for other passbands.en
dc.format.extent18
dc.format.extent4075743
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectastro-ph.SR
dc.subjectSolar neighbourhood
dc.subjectBinaries: visual
dc.subjectHertzsprung–Russell and colour–magnitude diagrams
dc.subjectBrown dwarfs
dc.subjectStars: late-type
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleThe Gaia Ultra-Cool Dwarf Sample -- II : Structure at the end of the main sequenceen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research (CAR)
dc.contributor.institutionCentre of Data Innovation Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85071970569&partnerID=8YFLogxK
rioxxterms.versionofrecord10.1093/mnras/stz678
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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