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dc.contributor.authorSkowron, J.
dc.contributor.authorUdalski, A.
dc.contributor.authorPoleski, R.
dc.contributor.authorKozłowski, S.
dc.contributor.authorSzymański, M. K.
dc.contributor.authorWyrzykowski, Ł.
dc.contributor.authorUlaczyk, K.
dc.contributor.authorPietrukowicz, P.
dc.contributor.authorPietrzyński, G.
dc.contributor.authorSoszyński, I.
dc.contributor.authorAbe, F.
dc.contributor.authorBennett, D. P.
dc.contributor.authorBhattacharya, A.
dc.contributor.authorBond, I. A.
dc.contributor.authorFreeman, M.
dc.contributor.authorFukui, A.
dc.contributor.authorHirao, Y.
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.authorNagakane, M.
dc.contributor.authorOhnishi, K.
dc.contributor.authorRattenbury, N.
dc.contributor.authorSaito, To
dc.contributor.authorSullivan, D. J.
dc.contributor.authorSumi, T.
dc.contributor.authorSuzuki, D.
dc.contributor.authorTristram, P. J.
dc.contributor.authorYonehara, A.
dc.contributor.authorDominik, Martin
dc.contributor.authorJørgensen, U. G.
dc.contributor.authorBozza, V.
dc.contributor.authorHarpsøe, K.
dc.contributor.authorHundertmark, M.
dc.contributor.authorSkottfelt, J.
dc.date.accessioned2016-04-22T08:37:34Z
dc.date.available2016-04-22T08:37:34Z
dc.date.issued2016-03-10
dc.identifier.citationSkowron , J , Udalski , A , Poleski , R , Kozłowski , S , Szymański , M K , Wyrzykowski , Ł , Ulaczyk , K , Pietrukowicz , P , Pietrzyński , G , Soszyński , I , Abe , F , Bennett , D P , Bhattacharya , A , Bond , I A , Freeman , M , Fukui , A , Hirao , Y , Itow , Y , Koshimoto , N , Ling , C H , Masuda , K , Matsubara , Y , Muraki , Y , Nagakane , M , Ohnishi , K , Rattenbury , N , Saito , T , Sullivan , D J , Sumi , T , Suzuki , D , Tristram , P J , Yonehara , A , Dominik , M , Jørgensen , U G , Bozza , V , Harpsøe , K , Hundertmark , M & Skottfelt , J 2016 , ' MOA-2011-BLG-028Lb : a Neptune-mass microlensing planet in the Galactic bulge ' , Astrophysical Journal , vol. 820 , no. 1 , 4 . https://doi.org/10.3847/0004-637X/820/1/4en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 242077081
dc.identifier.otherPURE UUID: 9b6ba756-9770-46c4-8982-4968015e7406
dc.identifier.otherScopus: 84962246343
dc.identifier.otherWOS: 000372787000004
dc.identifier.otherORCID: /0000-0002-3202-0343/work/75996773
dc.identifier.urihttp://hdl.handle.net/10023/8665
dc.descriptionThe OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U.. J.S. was partially supported by the Space Exploration Research Fund of The Ohio State University. This research was partly supported by the Polish Ministry of Science and Higher Education (MNiSW) through the program "Iuventus Plus" award No. IP2011 026771. We thank Prof. M. Kubiak for contributing observations to this work as the OGLE Project member. T.S. acknowledges the financial support from the JSPS, JSPS23103002, JSPS24253004, and JSPS26247023. The MOA project is supported by the grants JSPS25103508 and 23340064.en
dc.description.abstractWe present the discovery of a Neptune-mass planet orbiting a star 0.8 ± 0.3M in the Galactic bulge. The planet manifested itself during the microlensing event MOA-2011-BLG-028/OGLE-2011-BLG-0203 as a low-mass companion to the lens star. The analysis of the light curve provides the measurement of the mass ratio (1.2 ± 0.2) × 10-4 , which indicates that the mass of the planet is 12–60 Earth masses. The lensing system is located at 7.3 ± 0.7 kpc away from the Earth near the direction of Baade's Window. The projected separation of the planet at the time of the microlensing event was 3.1–5.2 au. Although the microlens parallax effect is not detected in the light curve of this event, preventing the actual mass measurement, the uncertainties of mass and distance estimation are narrowed by the measurement of the source star proper motion on the OGLE-III images spanning eight years, and by the low amount of blended light seen, proving that the host star cannot be too bright and massive. We also discuss the inclusion of undetected parallax and orbital motion effects into the models and their influence onto the final physical parameters estimates.preventing the actual mass measurement, the uncertainties of mass and distance estimation are narrowed by the measurement of the source star proper motion on the OGLE-III images spanning eight years, and by the low amount of blended light seen, proving that the host star cannot be too bright and massive. We also discuss the inclusion of undetected parallax and orbital motion effects into the models and their influence onto the final physical parameters estimates.
dc.format.extent13
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2016. 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: https://dx.doi.org/10.3847/0004-637X/820/1/4en
dc.subjectGravitational lensing: microen
dc.subjectPlanetary systemsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectSpace and Planetary Scienceen
dc.subjectAstronomy and Astrophysicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleMOA-2011-BLG-028Lb : a Neptune-mass microlensing planet in the Galactic bulgeen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.3847/0004-637X/820/1/4
dc.description.statusPeer revieweden


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