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dc.contributor.authorZapatero Osorio, M R
dc.contributor.authorBéjar, V J S
dc.contributor.authorLodieu, N
dc.contributor.authorManjavacas, E
dc.date.accessioned2018-05-02T19:30:49Z
dc.date.available2018-05-02T19:30:49Z
dc.date.issued2018-03-21
dc.identifier.citationM R Zapatero Osorio, V J S Béjar, N Lodieu, E Manjavacas; Confirming the least massive members of the Pleiades star cluster, Monthly Notices of the Royal Astronomical Society, Volume 475, Issue 1, 21 March 2018, Pages 139–153, https://doi.org/10.1093/mnras/stx3154en_US
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.doi10.1093/mnras/stx3154
dc.identifier.urihttp://hdl.handle.net/10150/627559
dc.description.abstractWe present optical photometry (i and Z band) and low-resolution spectroscopy (640-1015 nm) of very faint candidate members (J = 20.2-21.2 mag) of the Pleiades star cluster (120 Myr). The main goal is to address their cluster membership via photometric, astrometric, and spectroscopic studies, and to determine the properties of the least massive population of the cluster through the comparison of the data with younger and older spectral counterparts and state-of-the art model atmospheres. We confirm three bona fide Pleiades members that have extremely red optical and infrared colours, effective temperatures of approximate to 1150 and approximate to 1350 K, and masses in the interval 11-20 M-jup, and one additional likely member that shares the same motion as the cluster but does not appear to be as red as the other members with similar brightness. This latter object requires further near-infrared spectroscopy to fully address its membership in the Pleiades. The optical spectra of two bona fide members were classified as L6-L7 and show features of K i, a tentative detection of Cs i, hydrides, and water vapour with an intensity similar to high-gravity dwarfs of related classification despite their young age. The properties of the Pleiades L6-L7 members clearly indicate that very red colours of L dwarfs are not a direct evidence of ages younger than approximate to 100Myr. We also report on the determination of the bolometric corrections for the coolest Pleiades members. These data can be used to interpret the observations of the atmospheres of exoplanets orbiting stars.en_US
dc.description.sponsorshipSpanish Ministry of Economy and Competitivity [AYA2016-79425-C3-2-P, AYA2015-69350-C3-2-P]en_US
dc.language.isoenen_US
dc.publisherOXFORD UNIV PRESSen_US
dc.relation.urlhttps://academic.oup.com/mnras/article/475/1/139/4705921en_US
dc.rights© 2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Societyen_US
dc.subjectbrown dwarfsen_US
dc.subjectstars: late typeen_US
dc.subjectstars: low massen_US
dc.subjectopen clusters and associations: individual: Pleiadesen_US
dc.titleConfirming the least massive members of the Pleiades star clusteren_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Dept Astron, Steward Observen_US
dc.identifier.journalMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETYen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleMonthly Notices of the Royal Astronomical Society
dc.source.volume475
dc.source.issue1
dc.source.beginpage139
dc.source.endpage153
refterms.dateFOA2018-05-02T19:30:50Z


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