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dc.contributor.authorLodieu, N.
dc.contributor.authorDeacon, N. R.
dc.contributor.authorHambly, N. C.
dc.date.accessioned2019-12-07T01:06:49Z
dc.date.available2019-12-07T01:06:49Z
dc.date.issued2012-05-01
dc.identifier.citationLodieu , N , Deacon , N R & Hambly , N C 2012 , ' Astrometric and photometric initial mass functions from the UKIDSS Galactic Clusters Survey - I. The Pleiades ' , Monthly Notices of the Royal Astronomical Society , vol. 422 , no. 2 , pp. 1495-1511 . https://doi.org/10.1111/j.1365-2966.2012.20723.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 10014215
dc.identifier.otherPURE UUID: e7c080be-3662-42fe-b615-42b5af2b27c4
dc.identifier.otherScopus: 84860235427
dc.identifier.urihttp://hdl.handle.net/2299/21967
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
dc.description.abstractWe present the results of a deep wide-field near-infrared survey of the entire Pleiades cluster recently released as part of the UKIRT Infrared Deep Sky Survey (UKIDSS) Galactic Clusters Survey (GCS) Data Release 9 (DR9). We have identified a sample of ∼1000 Pleiades cluster member candidates combining photometry in five near-infrared passbands and proper motions derived from the multiple epochs provided by the UKIDSS GCS DR9. We also provide revised membership for all previously published Pleiades low-mass stars and brown dwarfs in the past decade recovered in the UKIDSS GCS DR9 Pleiades survey based on the new photometry and astrometry provided by the GCS. We find no evidence of K-band variability in the Pleiades members larger than ∼0.08mag. In addition, we infer a substellar binary frequency of 22-31per cent in the 0.075-0.03M ⊙ range for separations less than ∼100au. We employed two independent but complementary methods to derive the cluster luminosity and mass functions: a probabilistic analysis and a more standard approach consisting of stricter astrometric and photometric cuts. We found that the resulting luminosity and mass functions obtained from both methods are very similar. We derive the Pleiades mass function in the 0.6-0.03M ⊙ range and found that it is best reproduced by a lognormal representation with a mean characteristic mass of 0.20 ± 0.05M ⊙, in agreement with earlier studies and the extrapolation of the field mass function.en
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectBrown dwarfs
dc.subjectInfrared: Stars
dc.subjectOpen clusters and associations: Individual: Pleiades
dc.subjectStars: Low-mass
dc.subjectStars: Luminosity function, mass function
dc.subjectTechniques: Photometric
dc.subjectSpace and Planetary Science
dc.subjectAstronomy and Astrophysics
dc.titleAstrometric and photometric initial mass functions from the UKIDSS Galactic Clusters Survey - I. The Pleiadesen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=84860235427&partnerID=8YFLogxK
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2012.20723.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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