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dc.contributor.authorDominik, M.
dc.contributor.authorBachelet, E.
dc.contributor.authorBozza, V.
dc.contributor.authorStreet, R. A.
dc.contributor.authorHan, C.
dc.contributor.authorHundertmark, M.
dc.contributor.authorUdalski, A.
dc.contributor.authorBramich, D. M.
dc.contributor.authorAlsubai, K. A.
dc.contributor.authorCalchi Novati, S.
dc.contributor.authorCiceri, S.
dc.contributor.authorD'Ago, G.
dc.contributor.authorJaimes, R. Figuera
dc.contributor.authorHaugbølle, T.
dc.contributor.authorHinse, T. C.
dc.contributor.authorHorne, K.
dc.contributor.authorJørgensen, U. G.
dc.contributor.authorJuncher, D.
dc.contributor.authorKains, N.
dc.contributor.authorKorhonen, H.
dc.contributor.authorMancini, L.
dc.contributor.authorMenzies, J.
dc.contributor.authorPopovas, A.
dc.contributor.authorRabus, M.
dc.contributor.authorRahvar, S.
dc.contributor.authorScarpetta, G.
dc.contributor.authorSchmidt, R.
dc.contributor.authorSkottfelt, J.
dc.contributor.authorSnodgrass, C.
dc.contributor.authorSouthworth, J.
dc.contributor.authorStarkey, D.
dc.contributor.authorSteele, I. A.
dc.contributor.authorSurdej, J.
dc.contributor.authorTsapras, Y.
dc.contributor.authorWambsganss, J.
dc.contributor.authorWertz, O.
dc.contributor.authorPietrukowicz, P.
dc.contributor.authorSzymański, M. K.
dc.contributor.authorMróz, P.
dc.contributor.authorSkowron, J.
dc.contributor.authorSoszyński, I.
dc.contributor.authorUlaczyk, K.
dc.contributor.authorPoleski, R.
dc.contributor.authorWyrzykowski, Ł.
dc.contributor.authorKozłowski, S.
dc.date.accessioned2019-02-19T17:30:05Z
dc.date.available2019-02-19T17:30:05Z
dc.date.issued2019-04-21
dc.identifier.citationDominik , M , Bachelet , E , Bozza , V , Street , R A , Han , C , Hundertmark , M , Udalski , A , Bramich , D M , Alsubai , K A , Calchi Novati , S , Ciceri , S , D'Ago , G , Jaimes , R F , Haugbølle , T , Hinse , T C , Horne , K , Jørgensen , U G , Juncher , D , Kains , N , Korhonen , H , Mancini , L , Menzies , J , Popovas , A , Rabus , M , Rahvar , S , Scarpetta , G , Schmidt , R , Skottfelt , J , Snodgrass , C , Southworth , J , Starkey , D , Steele , I A , Surdej , J , Tsapras , Y , Wambsganss , J , Wertz , O , Pietrukowicz , P , Szymański , M K , Mróz , P , Skowron , J , Soszyński , I , Ulaczyk , K , Poleski , R , Wyrzykowski , Ł & Kozłowski , S 2019 , ' OGLE-2014-BLG-1186 : gravitational microlensing providing evidence for a planet orbiting the foreground star or for a close binary source? ' , Monthly Notices of the Royal Astronomical Society , vol. 484 , no. 4 , pp. 5608-5632 . https://doi.org/10.1093/mnras/stz306en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 257778034
dc.identifier.otherPURE UUID: f2bab853-6654-47aa-9949-6f4c64bdacf5
dc.identifier.otherBibCode: 2019MNRAS.tmp..308D
dc.identifier.otherScopus: 85066975137
dc.identifier.otherWOS: 000462414400082
dc.identifier.otherORCID: /0000-0002-3202-0343/work/75996734
dc.identifier.urihttp://hdl.handle.net/10023/17097
dc.descriptionFunding: UK STFC grant ST/R000824/1 (KH).en
dc.description.abstractDiscussing the particularly long gravitational microlensing event OGLE-2014-BLG-1186 with a time-scale tE ∼ 300 d, we present a methodology for identifying the nature of localised deviations from single-lens point-source light curves, which ensures that (1) the claimed signal is substantially above the noise floor, (2) the inferred properties are robustly determined and their estimation is not subject to confusion with systematic noise in the photometry, (3) alternative viable solutions within the model framework are not missed. Annual parallax and binarity could be separated and robustly measured from the wing and the peak data, respectively. We find matching model light curves that involve either a binary lens or a binary source, and discover hitherto unknown model ambiguities. Our binary-lens models indicate a planet of mass M2 = (45 ± 9) M⊕, orbiting a star of mass M1 = (0.35 ± 0.06) M⊙, located at a distance DL = (1.7 ± 0.3) kpc from Earth, whereas our binary-source models suggest a brown-dwarf lens of M = (0.046 ± 0.007) M⊙, located at a distance DL = (5.7 ± 0.9) kpc, with the source potentially being a (partially) eclipsing binary involving stars predicted to be of similar colour given the ratios between the luminosities and radii. Further observations might resolve the ambiguity in the interpretation in favour of either a lens or a source binary. We experienced that close binary source stars pose a challenge for claiming the detection of planets by microlensing in events where the source passes very close to the lens star hosting the planet.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2019, the Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with the publisher's policies. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stz306en
dc.subjectGravitational lensing: microen
dc.subjectMethods: data analysisen
dc.subjectMethods: statisticalen
dc.subjectPlanets and satellites: detectionen
dc.subject(Stars:) binaries: eclipsingen
dc.subjectGalaxy: kinematics and dynamicsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleOGLE-2014-BLG-1186 : gravitational microlensing providing evidence for a planet orbiting the foreground star or for a close binary source?en
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/10.1093/mnras/stz306
dc.description.statusPeer revieweden


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