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dc.contributor.authorUdalski, A.
dc.contributor.authorHan, C.
dc.contributor.authorBozza, V.
dc.contributor.authorGould, A.
dc.contributor.authorBond, I. A.
dc.contributor.authorMróz, P.
dc.contributor.authorSkowron, J.
dc.contributor.authorWyrzykowski, Ł.
dc.contributor.authorSzymański, M. K.
dc.contributor.authorSoszyński, I.
dc.contributor.authorUlaczyk, K.
dc.contributor.authorPoleski, R.
dc.contributor.authorPietrukowicz, P.
dc.contributor.authorKozłowski, S.
dc.contributor.authorAbe, F.
dc.contributor.authorBarry, R.
dc.contributor.authorBennett, D. P.
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.authorKawasaki, K.
dc.contributor.authorKoshimoto, N.
dc.contributor.authorLi, M. C. A.
dc.contributor.authorLing, C. H.
dc.contributor.authorMasuda, K.
dc.contributor.authorMatsubara, Y.
dc.contributor.authorMiyazaki, S.
dc.contributor.authorMunakata, H.
dc.contributor.authorMuraki, Y.
dc.contributor.authorNagakane, M.
dc.contributor.authorOhnishi, K.
dc.contributor.authorRanc, C.
dc.contributor.authorRattenbury, N.
dc.contributor.authorSaito, T.
dc.contributor.authorSharan, A.
dc.contributor.authorSullivan, D. J.
dc.contributor.authorSumi, T.
dc.contributor.authorSuzuki, D.
dc.contributor.authorTristram, P. J.
dc.contributor.authorYamada, T.
dc.contributor.authorYonehara, A.
dc.contributor.authorBachelet, E.
dc.contributor.authorBramich, D. M.
dc.contributor.authorDÁgo, G.
dc.contributor.authorDominik, M.
dc.contributor.authorJaimes, R. Figuera
dc.contributor.authorHorne, K.
dc.contributor.authorHundertmark, M.
dc.contributor.authorKains, N.
dc.contributor.authorMenzies, J.
dc.contributor.authorSchmidt, R.
dc.contributor.authorSnodgrass, C.
dc.contributor.authorSteele, I. A.
dc.contributor.authorWambsganss, J.
dc.contributor.authorPogge, R. W.
dc.contributor.authorJung, Y. K.
dc.contributor.authorShin, I. -G.
dc.contributor.authorYee, J. C.
dc.contributor.authorKim, W. -T.
dc.contributor.authorBeichman, C.
dc.contributor.authorCarey, S.
dc.contributor.authorNovati, S. Calchi
dc.contributor.authorZhu, W.
dc.date.accessioned2018-01-31T10:30:16Z
dc.date.available2018-01-31T10:30:16Z
dc.date.issued2018-01-24
dc.identifier.citationUdalski , A , Han , C , Bozza , V , Gould , A , Bond , I A , Mróz , P , Skowron , J , Wyrzykowski , Ł , Szymański , M K , Soszyński , I , Ulaczyk , K , Poleski , R , Pietrukowicz , P , Kozłowski , S , Abe , F , Barry , R , Bennett , D P , Bhattacharya , A , Donachie , M , Evans , P , Fukui , A , Hirao , Y , Itow , Y , Kawasaki , K , Koshimoto , N , Li , M C A , Ling , C H , Masuda , K , Matsubara , Y , Miyazaki , S , Munakata , H , Muraki , Y , Nagakane , M , Ohnishi , K , Ranc , C , Rattenbury , N , Saito , T , Sharan , A , Sullivan , D J , Sumi , T , Suzuki , D , Tristram , P J , Yamada , T , Yonehara , A , Bachelet , E , Bramich , D M , DÁgo , G , Dominik , M , Jaimes , R F , Horne , K , Hundertmark , M , Kains , N , Menzies , J , Schmidt , R , Snodgrass , C , Steele , I A , Wambsganss , J , Pogge , R W , Jung , Y K , Shin , I -G , Yee , J C , Kim , W -T , Beichman , C , Carey , S , Novati , S C & Zhu , W 2018 , ' OGLE-2014-BLG-0289 : precise characterization of a quintuple-peak gravitational microlensing event ' , Astrophysical Journal , vol. 853 , no. 1 , 70 . https://doi.org/10.3847/1538-4357/aaa295en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 252150098
dc.identifier.otherPURE UUID: b7311db3-048f-4e17-a847-3d46bf3ae96f
dc.identifier.otherArXiv: http://arxiv.org/abs/1801.05084v1
dc.identifier.otherScopus: 85041112464
dc.identifier.otherWOS: 000423361100006
dc.identifier.otherORCID: /0000-0002-3202-0343/work/75996695
dc.identifier.urihttps://hdl.handle.net/10023/12640
dc.description.abstractWe present the analysis of the binary-microlensing event OGLE-2014-BLG-0289. The event light curve exhibits five very unusual peaks, four of which were produced by caustic crossings and the other by a cusp approach. It is found that the quintuple-peak features of the light curve provide tight constraints on the source trajectory, enabling us to precisely and accurately measure the microlensing parallax πE. Furthermore, the three resolved caustics allow us to measure the angular Einstein radius θE. From the combination of πE and θE, the physical lens parameters are uniquely determined. It is found that the lens is a binary composed of two M dwarfs with masses M1 = 0.52 ± 0.04 M⊙ and M2 = 0.42 ± 0.03 M⊙ separated in projection by a⊥ = 6.4 ± 0.5 au. The lens is located in the disk with a distance of DL = 3.3 ± 0.3 kpc. The reason for the absence of a lensing signal in the Spitzer data is that the time of observation corresponds to the flat region of the light curve.
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2018, American 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/10.3847/1538-4357/aaa295en
dc.subjectBinaries: generalen
dc.subjectGravitational lensing: microen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleOGLE-2014-BLG-0289 : precise characterization of a quintuple-peak gravitational microlensing eventen
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/10.3847/1538-4357/aaa295
dc.description.statusPeer revieweden


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