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		<doi>10.1088/0004-637X/754/1/73</doi>
		<issn>0004-637X</issn>
		<issn>1538-4357</issn>
		<label>lattes: 7812463045514059 41 BacheletSHFGMBBBDHMMSSSUAAAABBBCCCCDDDGGHHHHJJKA:2012:COMAMI</label>
		<citationkey>BacheletSHFGMBBBDHMMSSSUAAAABBBCCCCDDDGGHHHHJJKAJ:2012:COMAMI</citationkey>
		<title>MOA 2010-BLG-477Lb: CONSTRAINING THE MASS OF A MICROLENSING PLANET FROM MICROLENSING PARALLAX, ORBITAL MOTION, AND DETECTION OF BLENDED LIGHT</title>
		<project>National Research Foundation of Korea [2009-0081561]; MOA [JSPS20340052, JSPS22403003]; Czech Science Foundation [GACR P209/10/1318]; French Polar Institute (IPEV); European Research Council under the European Community's Seventh Framework Programme/ERC [246678]; CALMIP [2011-P1131]; NSF [AST-1103471, 2009068160]; NASA [NNG04GL51G]; KRCF Young Scientist Research Fellowship Program in South Korea; ANR; CNRS; Observatoire de la Cote d'Azur; California Institute of Technology (Caltech); NASA; ANR HOLMES; ANR PNPS</project>
		<year>2012</year>
		<month>July</month>
		<secondarytype>PRE PI</secondarytype>
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		<author>Bachelet, E.,</author>
		<author>Shin, I. -G.,</author>
		<author>Han, C.,</author>
		<author>Fouqué, P.,</author>
		<author>Gould, A.,</author>
		<author>Menzies, J. W.,</author>
		<author>Beaulieu, J. -P.,</author>
		<author>Bennett, D. P.,</author>
		<author>Bond, I. A.,</author>
		<author>Dong, Subo,</author>
		<author>Heyrovsk, D.,</author>
		<author>Marquette, J. -B.,</author>
		<author>Marshall, J.,</author>
		<author>Skowron, J.,</author>
		<author>Street, R. A.,</author>
		<author>Sumi, T.,</author>
		<author>Udalski, A.,</author>
		<author>Abe, L.,</author>
		<author>Agabi, K.,</author>
		<author>Albrow, M. D.,</author>
		<author>Allen, W.,</author>
		<author>Bertin, E.,</author>
		<author>Bos, M.,</author>
		<author>Bramich, D. M.,</author>
		<author>Chavez, J.,</author>
		<author>Christie, G. W.,</author>
		<author>Cole, A. A.,</author>
		<author>Crouzet, N.,</author>
		<author>Dieters, S.,</author>
		<author>Dominik, M.,</author>
		<author>Drummond, J.,</author>
		<author>Greenhill, J.,</author>
		<author>Guillot, T.,</author>
		<author>Henderson, C. B.,</author>
		<author>Hessman, F. V.,</author>
		<author>Horne, K.,</author>
		<author>Hundertmark, M.,</author>
		<author>Johnson, J. A.,</author>
		<author>Jrgensen, U. G.,</author>
		<author>Kandori, R.,</author>
		<author>Almeida, Leonardo Andrade,</author>
		<author>Jablonski, F.,</author>
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		<group>DAS-CEA-INPE-MCTI-GOV-BR</group>
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		<affiliation>IRAP, Université de Toulouse, CNRS, 14 Avenue Edouard Belin, 31400 Toulouse, France</affiliation>
		<affiliation>Department of Physics, Chungbuk National University, Cheongju 361-763, Republic of Korea</affiliation>
		<affiliation>Department of Physics, Chungbuk National University, Cheongju 361-763, Republic of Korea</affiliation>
		<affiliation>IRAP, Université de Toulouse, CNRS, 14 Avenue Edouard Belin, 31400 Toulouse, France</affiliation>
		<affiliation>Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA</affiliation>
		<affiliation>South African Astronomical Observatory, P.O. Box 9, Observatory 7925, South Africa</affiliation>
		<affiliation>UPMC-CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98bis boulevard Arago, F-75014 Paris, France</affiliation>
		<affiliation>Department of Physics, 225 Nieuwland Science Hall, University of Notre Dame, Notre Dame, IN 46556, USA</affiliation>
		<affiliation>Institute for Information and Mathematical Sciences, Massey University, Private Bag 102-904, Auckland 1330, New Zealand</affiliation>
		<affiliation>Institute for Advanced Study, Einstein Drive, Princeton, NJ 08540, USA</affiliation>
		<affiliation>Institute of Theoretical Physics, Charles University, V Holešovi&#269;kách 2, 18000 Prague, Czech Republic</affiliation>
		<affiliation>UPMC-CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98bis boulevard Arago, F-75014 Paris, France</affiliation>
		<affiliation>Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA</affiliation>
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		<affiliation>Instituto Nacional de Pesquisas Espaciais (INPE)</affiliation>
		<affiliation>Instituto Nacional de Pesquisas Espaciais (INPE)</affiliation>
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		<electronicmailaddress>leonardo@das.inpe.br</electronicmailaddress>
		<e-mailaddress>leonardo@das.inpe.br</e-mailaddress>
		<journal>Astrophysical Journal</journal>
		<volume>754</volume>
		<number>1</number>
		<pages>73</pages>
		<secondarymark>A1_ASTRONOMIA_/_FÍSICA A2_ENGENHARIAS_IV A1_GEOCIÊNCIAS</secondarymark>
		<transferableflag>1</transferableflag>
		<contenttype>External Contribution</contenttype>
		<versiontype>publisher</versiontype>
		<keywords>gravitational lensing: micro, planetary systems.</keywords>
		<abstract>Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA 2010-BLG-477. The measured planet-star mass ratio is q = (2.181 +/- 0.004) x 10(-3) and the projected separation is s = 1.1228 +/- 0.0006 in units of the Einstein radius. The angular Einstein radius is unusually large theta(E) = 1.38 +/- 0.11 mas. Combining this measurement with constraints on the "microlens parallax" and the lens flux, we can only limit the host mass to the range 0.13 < M/M-circle dot < 1.0. In this particular case, the strong degeneracy between microlensing parallax and planet orbital motion prevents us from measuring more accurate host and planet masses. However, we find that adding Bayesian priors from two effects (Galactic model and Keplerian orbit) each independently favors the upper end of this mass range, yielding star and planet masses of M-* = 0.67(-0.13)(+0.33) M-circle dot and m(p) = 1.5(-0.3)(+0.8) M-JUP at a distance of D = 2.3 +/- 0.6 kpc, and with a semi-major axis of a = 2(-1)(+3) AU. Finally, we show that the lens mass can be determined from future high-resolution near-IR adaptive optics observations independently from two effects, photometric and astrometric.</abstract>
		<area>CEA</area>
		<language>pt</language>
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