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dc.contributor.authorBennett, D. P.
dc.contributor.authorUdalski, A.
dc.contributor.authorHan, C.
dc.contributor.authorBond, I. A.
dc.contributor.authorBeaulieu, J. -P.
dc.contributor.authorSkowron, J.
dc.contributor.authorGaudi, B. S.
dc.contributor.authorKoshimoto, N.
dc.contributor.authorAbe, F.
dc.contributor.authorAsakura, Y.
dc.contributor.authorBarry, R. K.
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.authorMuraki, Y.
dc.contributor.authorNagakane, M.
dc.contributor.authorOhnishi, K.
dc.contributor.authorOyokawa, H.
dc.contributor.authorRanc, C.
dc.contributor.authorRattenbury, N. J.
dc.contributor.authorRosenthal, M. K.
dc.contributor.authorSaito, To
dc.contributor.authorSharan, A.
dc.contributor.authorSullivan, D. J.
dc.contributor.authorSumi, T.
dc.contributor.authorSuzuki, D.
dc.contributor.authorTristram, P. J.
dc.contributor.authorYonehara, A.
dc.contributor.authorSzymański, M. K.
dc.contributor.authorPoleski, R.
dc.contributor.authorSoszyński, I.
dc.contributor.authorUlaczyk, K.
dc.contributor.authorWyrzykowski, Ł.
dc.contributor.authorDePoy, D.
dc.contributor.authorGould, A.
dc.contributor.authorPogge, R. W.
dc.contributor.authorYee, J. C.
dc.contributor.authorAlbrow, M. D.
dc.contributor.authorBachelet, E.
dc.contributor.authorBatista, V.
dc.contributor.authorBowens-Rubin, R.
dc.contributor.authorBrillant, S.
dc.contributor.authorCaldwell, J. A. R.
dc.contributor.authorCole, A.
dc.contributor.authorCoutures, C.
dc.contributor.authorDieters, S.
dc.contributor.authorPrester, D. Dominis
dc.contributor.authorDonatowicz, J.
dc.contributor.authorFouquė, P.
dc.contributor.authorHorne, K.
dc.contributor.authorHundertmark, M.
dc.contributor.authorKains, N.
dc.contributor.authorKane, S. R.
dc.contributor.authorMarquette, J. -B.
dc.contributor.authorMenzies, J.
dc.contributor.authorPollard, K. R.
dc.contributor.authorRanc, C.
dc.contributor.authorSahu, K. C.
dc.contributor.authorWambsganss, J.
dc.contributor.authorWilliams, A.
dc.contributor.authorZub, M.
dc.date.accessioned2018-03-16T15:30:06Z
dc.date.available2018-03-16T15:30:06Z
dc.date.issued2018-03
dc.identifier.citationBennett , D P , Udalski , A , Han , C , Bond , I A , Beaulieu , J -P , Skowron , J , Gaudi , B S , Koshimoto , N , Abe , F , Asakura , Y , Barry , R K , Bhattacharya , A , Donachie , M , Evans , P , Fukui , A , Hirao , Y , Itow , Y , Li , M C A , Ling , C H , Masuda , K , Matsubara , Y , Muraki , Y , Nagakane , M , Ohnishi , K , Oyokawa , H , Ranc , C , Rattenbury , N J , Rosenthal , M K , Saito , T , Sharan , A , Sullivan , D J , Sumi , T , Suzuki , D , Tristram , P J , Yonehara , A , Szymański , M K , Poleski , R , Soszyński , I , Ulaczyk , K , Wyrzykowski , Ł , DePoy , D , Gould , A , Pogge , R W , Yee , J C , Albrow , M D , Bachelet , E , Batista , V , Bowens-Rubin , R , Brillant , S , Caldwell , J A R , Cole , A , Coutures , C , Dieters , S , Prester , D D , Donatowicz , J , Fouquė , P , Horne , K , Hundertmark , M , Kains , N , Kane , S R , Marquette , J -B , Menzies , J , Pollard , K R , Ranc , C , Sahu , K C , Wambsganss , J , Williams , A & Zub , M 2018 , ' The first planetary microlensing event with two microlensed source stars ' Astronomical Journal , vol. 155 , no. 3 , 141 . DOI: 10.3847/1538-3881/aaadfaen
dc.identifier.issn0004-6256
dc.identifier.otherPURE: 252572002
dc.identifier.otherPURE UUID: bd3e5111-96c1-4079-9995-0bec0d92dea9
dc.identifier.otherArXiv: http://arxiv.org/abs/1707.09667v2
dc.identifier.otherScopus: 85043604182
dc.identifier.urihttp://hdl.handle.net/10023/12961
dc.description.abstractWe present the analysis of the microlensing event MOA-2010-BLG-117, and show that the light curve can only be explained by the gravitational lensing of a binary source star system by a star with a Jupiter-mass ratio planet. It was necessary to modify standard microlensing modeling methods to find the correct light curve solution for this binary source, binary-lens event. We are able to measure a strong microlensing parallax signal, which yields the masses of the host star, M * = 0.58 ± 0.11 M ⊙, and planet, mp = 0.54 ± 0.10MJup, at a projected star–planet separation of a ⊥ = 2.42 ± 0.26 au, corresponding to a semimajor axis of a = 2.9 (^+1.6_-0.6) au. Thus, the system resembles a half-scale model of the Sun–Jupiter system with a half-Jupiter0mass planet orbiting a half-solar-mass star at very roughly half of Jupiter's orbital distance from the Sun. The source stars are slightly evolved, and by requiring them to lie on the same isochrone, we can constrain the source to lie in the near side of the bulge at a distance of DS = 6.9 ± 0.7 kpc, which implies a distance to the planetary lens system of DL = 3.5 ± 0.4 kpc. The ability to model unusual planetary microlensing events, like this one, will be necessary to extract precise statistical information from the planned large exoplanet microlensing surveys, such as the WFIRST microlensing survey.en
dc.format.extent15en
dc.language.isoeng
dc.relation.ispartofAstronomical Journalen
dc.rights© 2018, The 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 https://doi.org/https://doi.org/10.3847/1538-3881/aaadfaen
dc.subjectGravitational lensing: microen
dc.subjectPlanetary systemsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe first planetary microlensing event with two microlensed source starsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.3847/1538-3881/aaadfa
dc.description.statusPeer revieweden


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