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dc.contributor.authorMancini, L.
dc.contributor.authorGiacobbe, P.
dc.contributor.authorLittlefair, S. P.
dc.contributor.authorSouthworth, J.
dc.contributor.authorBozza, V.
dc.contributor.authorDamasso, M.
dc.contributor.authorDominik, Martin
dc.contributor.authorHundertmark, Markus Peter Gerhard
dc.contributor.authorJørgensen, U. G.
dc.contributor.authorJuncher, Diana
dc.contributor.authorPopovas, A.
dc.contributor.authorRabus, M.
dc.contributor.authorRahvar, S.
dc.contributor.authorSchmidt, R. W.
dc.contributor.authorSkottfelt, J.
dc.contributor.authorSnodgrass, C.
dc.contributor.authorSozzetti, A.
dc.contributor.authorAlsubai, K.
dc.contributor.authorBramich, D. M.
dc.contributor.authorCalchi Novati, S.
dc.contributor.authorCiceri, S.
dc.contributor.authorD'Ago, G.
dc.contributor.authorFiguera Jaimes, Roberto Jose
dc.contributor.authorGalianni, P.
dc.contributor.authorGu, S.-H.
dc.contributor.authorHarpsøe, K.
dc.contributor.authorHaugbølle, T.
dc.contributor.authorHenning, Th.
dc.contributor.authorHinse, T. C.
dc.contributor.authorKains, Noé
dc.contributor.authorKorhonen, H.
dc.contributor.authorScarpetta, G.
dc.contributor.authorStarkey, David
dc.contributor.authorSurdej, J.
dc.contributor.authorWang, X.-B.
dc.contributor.authorWertz, O.
dc.date.accessioned2016-02-02T15:10:06Z
dc.date.available2016-02-02T15:10:06Z
dc.date.issued2015-12-01
dc.identifier.citationMancini , L , Giacobbe , P , Littlefair , S P , Southworth , J , Bozza , V , Damasso , M , Dominik , M , Hundertmark , M P G , Jørgensen , U G , Juncher , D , Popovas , A , Rabus , M , Rahvar , S , Schmidt , R W , Skottfelt , J , Snodgrass , C , Sozzetti , A , Alsubai , K , Bramich , D M , Calchi Novati , S , Ciceri , S , D'Ago , G , Figuera Jaimes , R J , Galianni , P , Gu , S-H , Harpsøe , K , Haugbølle , T , Henning , T , Hinse , T C , Kains , N , Korhonen , H , Scarpetta , G , Starkey , D , Surdej , J , Wang , X-B & Wertz , O 2015 , ' Rotation periods and astrometric motions of the Luhman 16AB brown dwarfs by high-resolution lucky-imaging monitoring ' Astronomy & Astrophysics , vol. 584 , A104 . DOI: 10.1051/0004-6361/201526899en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 240080516
dc.identifier.otherPURE UUID: 79c90cd5-9e3c-42ed-8b84-26ba17b8e242
dc.identifier.otherBibCode: 2015A&A...584A.104M
dc.identifier.otherScopus: 84949192141
dc.identifier.urihttp://hdl.handle.net/10023/8115
dc.identifier.urihttp://adsabs.harvard.edu/abs/2015A%26A...584A.104Men
dc.descriptionJ. Southworth acknowledges financial support from the STFC in the form of an Advanced Fellowship. O.W. and J. Surdej acknowledge support from the Communauté française de Belgique – Actions de recherche concertées – Académie Wallonie-Europe. S.H.G. and X.B.W. would like to acknowledge the financial support from the National Natural Science Foundation of China through grants Nos. 10873031 and 11473066. M.H. acknowledges support from the Villum Foundation.en
dc.description.abstractContext. Photometric monitoring of the variability of brown dwarfs canprovide useful information about the structure of clouds in their cold atmospheres.The brown-dwarf binary system Luhman 16AB is an interesting target for such a study, because its components stand at the L/Ttransition and show high levels of variability. Luhman 16AB is also the third closest system to the solar system, which allows precise astrometric investigations with ground-based facilities. Aims. The aim of the work is to estimate the rotation period and study theastrometric motion of both components. Methods. We have monitored Luhman 16AB over a period of two years with the lucky-imaging camera mounted on the Danish 1.54 m telescope at La Silla, through a special i + z long-pass filter, which allowed us to clearly resolve the two brown dwarfs into single objects. An intense monitoring of the target was also performed over 16 nights, in which we observed a peak-to-peak variability of 0.20 ± 0.02 mag and 0.34 ± 0.02 mag for Luhman 16A and 16B, respectively. Results. We used the 16-night time-series data to estimate the rotation period of the two components. We found that Luhman 16B rotates with a period of 5.1 ± 0.1 h, in very good agreement with previous measurements. For Luhman 16A, we report that it rotates more slowly than its companion, and even though we were not able to get a robust determination, our data indicate a rotation period of roughly 8 h. This implies that the rotation axes of the two components are well aligned and suggests a scenario in which the two objects underwent the same accretion process. The 2-year complete data set was used to study the astrometric motion of Luhman 16AB. We predict a motion of the system that is not consistent with a previous estimate based on two months of monitoring, but cannot confirm or refute the presence of additional planetary-mass bodies in the system.en
dc.format.extent9en
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© ESO, 2015. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at http://dx.doi.org/10.1051/0004-6361/201526899.en
dc.subjectBinaries: visualen
dc.subjectBrown dwarfsen
dc.subjectStars: variables: generalen
dc.subjectTechniques: photometricen
dc.subjectTechniques: image processingen
dc.subjectQC Physicsen
dc.subjectQB Astronomyen
dc.subjectNDASen
dc.subject.lccQCen
dc.subject.lccQBen
dc.titleRotation periods and astrometric motions of the Luhman 16AB brown dwarfs by high-resolution lucky-imaging monitoringen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201526899
dc.description.statusPeer revieweden


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