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dc.contributor.authorSkowron, J.
dc.contributor.authorShin, I.
dc.contributor.authorUdalski, A.
dc.contributor.authorHan, C.
dc.contributor.authorSumi, T.
dc.contributor.authorShvartzvald, Y.
dc.contributor.authorGould, A.
dc.contributor.authorDominis Prester, D.
dc.contributor.authorStreet, R.
dc.contributor.authorJorgensen, U.
dc.contributor.authorBennett, D.
dc.contributor.authorBozza, V.
dc.contributor.authorSzymanski, M.
dc.contributor.authorKubiak, M.
dc.contributor.authorPietrzynski, G.
dc.contributor.authorSoszynski, I.
dc.contributor.authorPoleski, R.
dc.contributor.authorKozlowski, S.
dc.contributor.authorPietrukowicz, P.
dc.contributor.authorUlaczyk, K.
dc.contributor.authorAbe, F.
dc.contributor.authorBhattacharya, A.
dc.contributor.authorBond, I.
dc.contributor.authorBotzler, C.
dc.contributor.authorFreeman, M.
dc.contributor.authorFukui, A.
dc.contributor.authorFukunaga, D.
dc.contributor.authorItow, Y.
dc.contributor.authorLing, C.
dc.contributor.authorKoshimoto, N.
dc.contributor.authorMasuda, K.
dc.contributor.authorMatsubara, Y.
dc.contributor.authorMuraki, Y.
dc.contributor.authorNamba, S.
dc.contributor.authorOhnishi, K.
dc.contributor.authorPhilpott, L.
dc.contributor.authorRattenbury, N.
dc.contributor.authorSaito, T.
dc.contributor.authorSullivan, D.
dc.contributor.authorSuzuki, D.
dc.contributor.authorTristram, P.
dc.contributor.authorYock, P.
dc.contributor.authorMaoz, D.
dc.contributor.authorKaspi, S.
dc.contributor.authorFriedmann, M.
dc.contributor.authorAlmeida, L.
dc.contributor.authorBatista, V.
dc.contributor.authorChristie, G.
dc.contributor.authorChoi, J.
dc.contributor.authorDepoy, D.
dc.contributor.authorGaudi, B.
dc.contributor.authorHenderson, C.
dc.contributor.authorHwang, K.
dc.contributor.authorJablonski, F.
dc.contributor.authorJung, Y.
dc.contributor.authorLee, C.
dc.contributor.authorMcCormick, J.
dc.contributor.authorNatusch, T.
dc.contributor.authorNgan, H.
dc.contributor.authorPark, H.
dc.contributor.authorPogge, R.
dc.contributor.authorYee, J.
dc.contributor.authorAlbrow, M.
dc.contributor.authorBachelet, E.
dc.contributor.authorBeaulieu, J.
dc.contributor.authorBrillant, S.
dc.contributor.authorCaldwell, J.
dc.contributor.authorCassan, A.
dc.contributor.authorCole, A.
dc.contributor.authorCorrales, E.
dc.contributor.authorCoutures, C.
dc.contributor.authorDieters, S.
dc.contributor.authorDonatowicz, J.
dc.contributor.authorFouqué, P.
dc.contributor.authorGreenhill, J.
dc.contributor.authorKains, N.
dc.contributor.authorKane, S.
dc.contributor.authorKubas, D.
dc.contributor.authorMarquette, J.
dc.contributor.authorMartin, R.
dc.contributor.authorMenzies, J.
dc.contributor.authorPollard, K.
dc.contributor.authorRanc, C.
dc.contributor.authorSahu, K.
dc.contributor.authorWambsganss, J.
dc.contributor.authorWilliams, Andrew
dc.contributor.authorWouters, D.
dc.contributor.authorTsapras, Y.
dc.identifier.citationSkowron, J. and Shin, I. and Udalski, A. and Han, C. and Sumi, T. and Shvartzvald, Y. and Gould, A. et al. 2015. OGLE-2011-BLG-0265Lb: A jovian microlensing planet orbiting an m dwarf. Astrophysical Journal. 804 (1).

© 2015. The American Astronomical Society. All rights reserved. We report the discovery of a Jupiter-mass planet orbiting an M-dwarf star that gave rise to the microlensing event OGLE-2011-BLG-0265. Such a system is very rare among known planetary systems and thus the discovery is important for theoretical studies of planetary formation and evolution. High-cadence temporal coverage of the planetary signal, combined with extended observations throughout the event, allows us to accurately model the observed light curve. However, the final microlensing solution remains degenerate, yielding two possible configurations of the planet and the host star. In the case of the preferred solution, the mass of the planet is Mp = 0.9 ± 0.3 MJ, and the planet is orbiting a star with a mass M = 0.22 ± 0.06 M. The second possible configuration (2? away) consists of a planet with Mp = 0.6 ± 0.3 MJ and host star with M = 0.14 ± 0.06 M. The system is located in the Galactic disk 34 kpc toward the Galactic bulge. In both cases, with an orbit size of 1.52.0 AU, the planet is a cold Jupiterlocated well beyond the snow line of the host star. Currently available data make the secure selection of the correct solution difficult, but there are prospects for lifting the degeneracy with additional follow-up observations in the future, when the lens and source star separate.

dc.publisherInstitute of Physics Publishing
dc.titleOGLE-2011-BLG-0265Lb: A jovian microlensing planet orbiting an m dwarf
dc.typeJournal Article
dcterms.source.titleAstrophysical Journal
curtin.departmentCurtin Institute of Radio Astronomy (Engineering)
curtin.accessStatusFulltext not available

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