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dc.contributor.authorHenderson, C. B.
dc.contributor.authorPark, H.
dc.contributor.authorSumi, T.
dc.contributor.authorUdalski, A.
dc.contributor.authorGould, A.
dc.contributor.authorTsapras, Y.
dc.contributor.authorHan, C.
dc.contributor.authorGaudi, B. S.
dc.contributor.authorBozza, V.
dc.contributor.authorAbe, F.
dc.contributor.authorBennett, D. P.
dc.contributor.authorBond, I. A.
dc.contributor.authorBotzler, C. S.
dc.contributor.authorFreeman, M.
dc.contributor.authorFukui, A.
dc.contributor.authorFukunaga, D.
dc.contributor.authorItow, Y.
dc.contributor.authorKoshimoto, N.
dc.contributor.authorLing, C. H.
dc.contributor.authorMasuda, K.
dc.contributor.authorMatsubara, Y.
dc.contributor.authorMuraki, Y.
dc.contributor.authorNamba, S.
dc.contributor.authorOhnishi, K.
dc.contributor.authorRattenbury, N. J.
dc.contributor.authorSaito, To
dc.contributor.authorSullivan, D. J.
dc.contributor.authorSuzuki, D.
dc.contributor.authorSweatman, W. L.
dc.contributor.authorTristram, P. J.
dc.contributor.authorTsurumi, N.
dc.contributor.authorWada, K.
dc.contributor.authorYamai, N.
dc.contributor.authorYock, P. C. M.
dc.contributor.authorYonehara, A.
dc.contributor.authorSzymanski, M. K.
dc.contributor.authorKubiak, M.
dc.contributor.authorPietrzynski, G.
dc.contributor.authorSoszynski, I.
dc.contributor.authorSkowron, J.
dc.contributor.authorKozlowski, S.
dc.contributor.authorPoleski, R.
dc.contributor.authorBramich, Daniel Martyn
dc.contributor.authorBrowne, Paul
dc.contributor.authorDominik, Martin
dc.contributor.authorHorne, Keith Douglas
dc.contributor.authorHundertmark, Markus Peter Gerhard
dc.contributor.authorFiguera Jaimes, Roberto Jose
dc.contributor.authorKains, Noé
dc.contributor.authorStreet, Rachel Amanda
dc.contributor.authorMOA Collaboration
dc.contributor.authorOGLE Collaboration
dc.contributor.authorFUN Collaboration
dc.contributor.authorRoboNet Collaboration
dc.date.accessioned2015-09-29T08:40:02Z
dc.date.available2015-09-29T08:40:02Z
dc.date.issued2014-10-10
dc.identifier.citationHenderson , C B , Park , H , Sumi , T , Udalski , A , Gould , A , Tsapras , Y , Han , C , Gaudi , B S , Bozza , V , Abe , F , Bennett , D P , Bond , I A , Botzler , C S , Freeman , M , Fukui , A , Fukunaga , D , Itow , Y , Koshimoto , N , Ling , C H , Masuda , K , Matsubara , Y , Muraki , Y , Namba , S , Ohnishi , K , Rattenbury , N J , Saito , T , Sullivan , D J , Suzuki , D , Sweatman , W L , Tristram , P J , Tsurumi , N , Wada , K , Yamai , N , Yock , P C M , Yonehara , A , Szymanski , M K , Kubiak , M , Pietrzynski , G , Soszynski , I , Skowron , J , Kozlowski , S , Poleski , R , Bramich , D M , Browne , P , Dominik , M , Horne , K D , Hundertmark , M P G , Figuera Jaimes , R J , Kains , N , Street , R A , MOA Collaboration , OGLE Collaboration , FUN Collaboration & RoboNet Collaboration 2014 , ' Candidate gravitational microlensing events for future direct lens imaging ' , Astrophysical Journal , vol. 794 , no. 1 , 71 . https://doi.org/10.1088/0004-637X/794/1/71en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 157834646
dc.identifier.otherPURE UUID: 472d3aef-d1c3-4a55-81e9-0a31c76e40b2
dc.identifier.otherWOS: 000342581200071
dc.identifier.otherWOS: 000342581200071
dc.identifier.otherScopus: 84907311501
dc.identifier.otherORCID: /0000-0002-3202-0343/work/75996740
dc.identifier.urihttp://hdl.handle.net/10023/7559
dc.descriptionThis material is based upon work supported by the National Science Foundation (NSF) Graduate Research Fellowship Program under grant No. DGE-0822215, awarded to C.B.H., and an international travel allowance through the Graduate Research Opportunities Worldwide, also awarded to C.B.H. and taken to Cheongju, Korea. T.S. is supported by the grant JSPS23340044 and JSPS24253004. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A.U. Work by C.H. was supported by the Creative Research Initiative Program (2009-0081561) of the National Research Foundation of Korea. A.G. and B.S.G. acknowledge support from NSF AST-1103471 and from NASA grant NNX12AB99G. S.D. is supported by "The Strategic Priority Research Program—The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (Grant No. XDB09000000). Work by J.C.Y. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. M.D., K.H., M.H., C.S., R.A.S., and Y.T. acknowledge grant NPRP-09-476-1-78 from the Qatar National Research Fund (a member of the Qatar Foundation). This publication was made possible by NPRP grant #X-019-1-006 from the Qatar National Research Fund (a member of the Qatar Foundation).en
dc.description.abstractThe mass of the lenses giving rise to Galactic microlensing events can be constrained by measuring the relative lens-source proper motion and lens flux. The flux of the lens can be separated from that of the source, companions to the source, and unrelated nearby stars with high-resolution images taken when the lens and source are spatially resolved. For typical ground-based adaptive optics (AO) or space-based observations, this requires either inordinately long time baselines or high relative proper motions. We provide a list of microlensing events toward the Galactic bulge with high relative lens-source proper motion that are therefore good candidates for constraining the lens mass with future high-resolution imaging. We investigate all events from 2004 to 2013 that display detectable finite-source effects, a feature that allows us to measure the proper motion. In total, we present 20 events with μ ≥ 8 mas yr–1. Of these, 14 were culled from previous analyses while 6 are new, including OGLE-2004-BLG-368, MOA-2005-BLG-36, OGLE-2012-BLG-0211, OGLE-2012-BLG-0456, MOA-2012-BLG-532, and MOA-2013-BLG-029. In ≤12 yr from the time of each event the lens and source of each event will be sufficiently separated for ground-based telescopes with AO systems or space telescopes to resolve each component and further characterize the lens system. Furthermore, for the most recent events, comparison of the lens flux estimates from images taken immediately to those estimated from images taken when the lens and source are resolved can be used to empirically check the robustness of the single-epoch method currently being used to estimate lens masses for many events.
dc.format.extent11
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2014. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at http://dx.doi.org/10.1088/0004-637X/794/1/71en
dc.subjectBinaries: generalen
dc.subjectGravitational lensing: microen
dc.subjectGalactic bulgeen
dc.subjectBinary-lensen
dc.subjectChemical evolutionen
dc.subjectPlanetary companionen
dc.subjectOrbital motionen
dc.subjectOptical depthen
dc.subjectMass planeten
dc.subjectBrown dwarfen
dc.subjectOGLE-IIIen
dc.subjectParallaxen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleCandidate gravitational microlensing events for future direct lens imagingen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/794/1/71
dc.description.statusPeer revieweden


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