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dc.contributor.authorDeacon, Niall
dc.contributor.authorSchlieder, Joshua E.
dc.contributor.authorMurphy, Simon J.
dc.date.accessioned2016-04-27T16:07:49Z
dc.date.available2016-04-27T16:07:49Z
dc.date.issued2016-04-11
dc.identifier.citationDeacon , N , Schlieder , J E & Murphy , S J 2016 , ' A nearby young M dwarf with a wide, possibly planetary-mass companion ' , Monthly Notices of the Royal Astronomical Society , vol. 457 , no. 3 , pp. 3191-3199 . https://doi.org/10.1093/mnras/stw172
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 10015280
dc.identifier.otherPURE UUID: 76d018e4-1805-412f-a4a0-e38082159b8d
dc.identifier.otherArXiv: http://arxiv.org/abs/1601.06162v1
dc.identifier.otherScopus: 84976878598
dc.identifier.urihttp://hdl.handle.net/2299/17156
dc.description.abstractWe present the identification of two previously known young objects in the solar neighbourhood as a likely very wide binary. TYC 9486-927-1, an active, rapidly rotating early-M dwarf, and 2MASS J21265040-8140293, a low-gravity L3 dwarf previously identified as candidate members of the $\sim$45 Myr old Tucana Horologium association (TucHor). An updated proper motion measurement of the L3 secondary, and a detailed analysis of the pair's kinematics in the context of known nearby, young stars, reveals that they share common proper motion and are likely bound. New observations and analyses reveal the primary exhibits Li 6708~\AA~absorption consistent with M dwarfs younger than TucHor but older than the $\sim$10 Myr TW Hydra association yielding an age range of 10-45 Myr. A revised kinematic analysis suggests the space motions and positions of the pair are closer to, but not entirely in agreement with, the $\sim$24 Myr old $\beta$ Pictoris moving group. This revised 10-45 Myr age range yields a mass range of 11.6--15 M$_J$ for the secondary. It is thus likely 2MASS J21265040-8140293short is the widest orbit planetary mass object known ($>$4500AU) and its estimated mass, age, spectral type, and $T_{eff}$ are similar to the well-studied planet $\beta$ Pictoris b. Because of their extreme separation and youth, this low-mass pair provide an interesting case study for very wide binary formation and evolution.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectastro-ph.EP
dc.subjectastro-ph.SR
dc.titleA nearby young M dwarf with a wide, possibly planetary-mass companionen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stw172
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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