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dc.contributor.authorHan, C.
dc.contributor.authorCalchi Novati, S.
dc.contributor.authorUdalski, A.
dc.contributor.authorLee, C.-U.
dc.contributor.authorGould, A.
dc.contributor.authorBozza, V.
dc.contributor.authorMróz, P.
dc.contributor.authorPietrukowicz, P.
dc.contributor.authorSkowron, J.
dc.contributor.authorSzymański, M. K.
dc.contributor.authorPoleski, R.
dc.contributor.authorSoszyński, I.
dc.contributor.authorKozłowski, S.
dc.contributor.authorUlaczyk, K.
dc.contributor.authorPawlak, M.
dc.contributor.authorRybicki, K.
dc.contributor.authorIwanek, P.
dc.contributor.authorAlbrow, M. D.
dc.contributor.authorChung, S.-J.
dc.contributor.authorHwang, K.-H.
dc.contributor.authorJung, Y. K.
dc.contributor.authorRyu, Y.-H.
dc.contributor.authorShin, I.-G.
dc.contributor.authorShvartzvald, Y.
dc.contributor.authorYee, J. C.
dc.contributor.authorZang, W.
dc.contributor.authorZhu, W.
dc.contributor.authorCha, S.-M.
dc.contributor.authorKim, D.-J.
dc.contributor.authorKim, H.-W.
dc.contributor.authorKim, S.-L.
dc.contributor.authorLee, D.-J.
dc.contributor.authorLee, Y.
dc.contributor.authorPark, B.-G.
dc.contributor.authorPogge, R. W.
dc.contributor.authorKim, W.-T.
dc.contributor.authorBeichman, C.
dc.contributor.authorBryden, G.
dc.contributor.authorCarey, S.
dc.contributor.authorGaudi, B. S.
dc.contributor.authorHenderson, C. B.
dc.contributor.authorDominik, M.
dc.contributor.authorHelling, C.
dc.contributor.authorHundertmark, M.
dc.contributor.authorJørgensen, U. G.
dc.contributor.authorLonga-Peña, P.
dc.contributor.authorLowry, S.
dc.contributor.authorSajadian, S.
dc.contributor.authorBurgdorf, M. J.
dc.contributor.authorCampbell-White, J.
dc.contributor.authorCiceri, S.
dc.contributor.authorEvans, D. F.
dc.contributor.authorHaikala, L. K.
dc.contributor.authorHinse, T. C.
dc.contributor.authorRahvar, S.
dc.contributor.authorRabus, M.
dc.contributor.authorSnodgrass, C.
dc.identifier.citationHan , C , Calchi Novati , S , Udalski , A , Lee , C-U , Gould , A , Bozza , V , Mróz , P , Pietrukowicz , P , Skowron , J , Szymański , M K , Poleski , R , Soszyński , I , Kozłowski , S , Ulaczyk , K , Pawlak , M , Rybicki , K , Iwanek , P , Albrow , M D , Chung , S-J , Hwang , K-H , Jung , Y K , Ryu , Y-H , Shin , I-G , Shvartzvald , Y , Yee , J C , Zang , W , Zhu , W , Cha , S-M , Kim , D-J , Kim , H-W , Kim , S-L , Lee , D-J , Lee , Y , Park , B-G , Pogge , R W , Kim , W-T , Beichman , C , Bryden , G , Carey , S , Gaudi , B S , Henderson , C B , Dominik , M , Helling , C , Hundertmark , M , Jørgensen , U G , Longa-Peña , P , Lowry , S , Sajadian , S , Burgdorf , M J , Campbell-White , J , Ciceri , S , Evans , D F , Haikala , L K , Hinse , T C , Rahvar , S , Rabus , M & Snodgrass , C 2018 , ' OGLE-2017-BLG-0329L : a microlensing binary characterized with dramatically enhanced precision using data from space-based observations ' , Astrophysical Journal , vol. 859 , no. 2 , 82 .
dc.identifier.otherPURE: 253279857
dc.identifier.otherPURE UUID: 36828bbd-fce3-4839-a6d6-2dc0a194003d
dc.identifier.otherBibCode: 2018ApJ...859...82H
dc.identifier.otherScopus: 85048311758
dc.identifier.otherWOS: 000433172900005
dc.identifier.otherORCID: /0000-0002-3202-0343/work/75996696
dc.description.abstractMass measurements of gravitational microlenses require one to determine the microlens parallax π E, but precise π E measurement, in many cases, is hampered due to the subtlety of the microlens-parallax signal combined with the difficulty of distinguishing the signal from those induced by other higher-order effects. In this work, we present the analysis of the binary-lens event OGLE-2017-BLG-0329, for which π E is measured with a dramatically improved precision using additional data from space-based Spitzer observations. We find that while the parallax model based on the ground-based data cannot be distinguished from a zero-π E model at the 2σ level, the addition of the Spitzer data enables us to identify two classes of solutions, each composed of a pair of solutions according to the well-known ecliptic degeneracy. It is found that the space-based data reduce the measurement uncertainties of the north and east components of the microlens-parallax vector πE by factors ∼18 and ∼4, respectively. With the measured microlens parallax combined with the angular Einstein radius measured from the resolved caustic crossings, we find that the lens is composed of a binary with component masses of either (M 1, M 2) ∼ (1.1, 0.8) M ⊙ or ∼(0.4, 0.3) M ⊙ according to the two solution classes. The first solution is significantly favored but the second cannot be securely ruled out based on the microlensing data alone. However, the degeneracy can be resolved from adaptive optics observations taken ∼10 years after the event.
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 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
dc.subjectBinaries: generalen
dc.subjectGravitational lensing: microen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleOGLE-2017-BLG-0329L : a microlensing binary characterized with dramatically enhanced precision using data from space-based observationsen
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.description.statusPeer revieweden

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