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dc.contributor.authorKoshimoto, N.
dc.contributor.authorShvartzvald, Y.
dc.contributor.authorBennett, D. P.
dc.contributor.authorPenny, M. T.
dc.contributor.authorHundertmark, M.
dc.contributor.authorBond, I. A.
dc.contributor.authorZang, W. C.
dc.contributor.authorHenderson, C. B.
dc.contributor.authorSuzuki, D.
dc.contributor.authorRattenbury, N. J.
dc.contributor.authorSumi, T.
dc.contributor.authorAbe, F.
dc.contributor.authorAsakura, Y.
dc.contributor.authorBhattacharya, A.
dc.contributor.authorDonachie, M.
dc.contributor.authorEvans, P.
dc.contributor.authorFukui, A.
dc.contributor.authorHirao, Y.
dc.contributor.authorItow, Y.
dc.contributor.authorLi, M. C. A.
dc.contributor.authorLing, C. H.
dc.contributor.authorMasuda, K.
dc.contributor.authorMatsubara, Y.
dc.contributor.authorMatsuo, T.
dc.contributor.authorMuraki, Y.
dc.contributor.authorNagakane, M.
dc.contributor.authorOhnishi, K.
dc.contributor.authorRanc, C.
dc.contributor.authorSaito, To.
dc.contributor.authorSharan, A.
dc.contributor.authorShibai, H.
dc.contributor.authorSullivan, D. J.
dc.contributor.authorTristram, P. J.
dc.contributor.authorYamada, T.
dc.contributor.authorYamada, T.
dc.contributor.authorYonehara, A.
dc.contributor.authorGelino, C. R.
dc.contributor.authorBeichman, C.
dc.contributor.authorBeaulieu, J.-P.
dc.contributor.authorMarquette, J.-B.
dc.contributor.authorBatista, V.
dc.contributor.authorFriedmann, M.
dc.contributor.authorHallakoun, N.
dc.contributor.authorKaspi, S.
dc.contributor.authorMaoz, D.
dc.contributor.authorBryden, G.
dc.contributor.authorCalchi Novati, S.
dc.contributor.authorHowell, S. B.
dc.contributor.authorWang, T. S.
dc.contributor.authorMao, S.
dc.contributor.authorFouqué, P.
dc.contributor.authorKorhonen, H.
dc.contributor.authorJørgensen, U. G.
dc.contributor.authorStreet, R.
dc.contributor.authorTsapras, Y.
dc.contributor.authorDominik, M.
dc.contributor.authorKerins, E.
dc.contributor.authorCassan, A.
dc.contributor.authorSnodgrass, C.
dc.contributor.authorBachelet, E.
dc.contributor.authorBozza, V.
dc.contributor.authorBramich, D. M.
dc.date.accessioned2017-07-06T11:30:09Z
dc.date.available2017-07-06T11:30:09Z
dc.date.issued2017-07
dc.identifier.citationKoshimoto , N , Shvartzvald , Y , Bennett , D P , Penny , M T , Hundertmark , M , Bond , I A , Zang , W C , Henderson , C B , Suzuki , D , Rattenbury , N J , Sumi , T , Abe , F , Asakura , Y , Bhattacharya , A , Donachie , M , Evans , P , Fukui , A , Hirao , Y , Itow , Y , Li , M C A , Ling , C H , Masuda , K , Matsubara , Y , Matsuo , T , Muraki , Y , Nagakane , M , Ohnishi , K , Ranc , C , Saito , T , Sharan , A , Shibai , H , Sullivan , D J , Tristram , P J , Yamada , T , Yamada , T , Yonehara , A , Gelino , C R , Beichman , C , Beaulieu , J-P , Marquette , J-B , Batista , V , Friedmann , M , Hallakoun , N , Kaspi , S , Maoz , D , Bryden , G , Calchi Novati , S , Howell , S B , Wang , T S , Mao , S , Fouqué , P , Korhonen , H , Jørgensen , U G , Street , R , Tsapras , Y , Dominik , M , Kerins , E , Cassan , A , Snodgrass , C , Bachelet , E , Bozza , V & Bramich , D M 2017 , ' MOA-2016-BLG-227Lb: a massive planet characterized by combining light-curve analysis and Keck AO imaging ' , Astronomical Journal , vol. 154 , no. 1 , 3 . https://doi.org/10.3847/1538-3881/aa72e0en
dc.identifier.issn0004-6256
dc.identifier.otherPURE: 250441380
dc.identifier.otherPURE UUID: 07e49c51-eb32-4308-8ca1-8925c33c0f04
dc.identifier.otherBibCode: 2017AJ....154....3K
dc.identifier.otherScopus: 85024387849
dc.identifier.otherWOS: 000403443800001
dc.identifier.otherORCID: /0000-0002-3202-0343/work/75996769
dc.identifier.urihttps://hdl.handle.net/10023/11160
dc.description.abstractWe report the discovery of a microlensing planet — MOA-2016-BLG-227Lb — with a large planet/host mass ratio of q ≃ 9 × 10‑3. This event was located near the K2 Campaign 9 field that was observed by a large number of telescopes. As a result, the event was in the microlensing survey area of a number of these telescopes, and this enabled good coverage of the planetary light-curve signal. High angular resolution adaptive optics images from the Keck telescope reveal excess flux at the position of the source above the flux of the source star, as indicated by the light-curve model. This excess flux could be due to the lens star, but it could also be due to a companion to the source or lens star, or even an unrelated star. We consider all these possibilities in a Bayesian analysis in the context of a standard Galactic model. Our analysis indicates that it is unlikely that a large fraction of the excess flux comes from the lens, unless solar-type stars are much more likely to host planets of this mass ratio than lower mass stars. We recommend that a method similar to the one developed in this paper be used for other events with high angular resolution follow-up observations when the follow-up observations are insufficient to measure the lens–source relative proper motion.
dc.format.extent15
dc.language.isoeng
dc.relation.ispartofAstronomical Journalen
dc.rights© 2017, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at iopscience.iop.org / https://doi.org/10.3847/1538-3881/aa72e0en
dc.subjectGravitational lensing: microen
dc.subjectPlanetary systemsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleMOA-2016-BLG-227Lb: a massive planet characterized by combining light-curve analysis and Keck AO imagingen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.3847/1538-3881/aa72e0
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2017AJ....154....3Ken


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