%0 Journal Article
%4 dpi.inpe.br/plutao/2012/11.28.18.48.35
%2 dpi.inpe.br/plutao/2012/11.28.18.48.36
%@doi 10.1088/0004-637X/754/1/73
%@issn 0004-637X
%@issn 1538-4357
%F lattes: 7812463045514059 41 BacheletSHFGMBBBDHMMSSSUAAAABBBCCCCDDDGGHHHHJJKA:2012:COMAMI
%T MOA 2010-BLG-477Lb: CONSTRAINING THE MASS OF A MICROLENSING PLANET FROM MICROLENSING PARALLAX, ORBITAL MOTION, AND DETECTION OF BLENDED LIGHT
%D 2012
%8 July
%A Bachelet, E.,
%A Shin, I. -G.,
%A Han, C.,
%A Fouqué, P.,
%A Gould, A.,
%A Menzies, J. W.,
%A Beaulieu, J. -P.,
%A Bennett, D. P.,
%A Bond, I. A.,
%A Dong, Subo,
%A Heyrovsk, D.,
%A Marquette, J. -B.,
%A Marshall, J.,
%A Skowron, J.,
%A Street, R. A.,
%A Sumi, T.,
%A Udalski, A.,
%A Abe, L.,
%A Agabi, K.,
%A Albrow, M. D.,
%A Allen, W.,
%A Bertin, E.,
%A Bos, M.,
%A Bramich, D. M.,
%A Chavez, J.,
%A Christie, G. W.,
%A Cole, A. A.,
%A Crouzet, N.,
%A Dieters, S.,
%A Dominik, M.,
%A Drummond, J.,
%A Greenhill, J.,
%A Guillot, T.,
%A Henderson, C. B.,
%A Hessman, F. V.,
%A Horne, K.,
%A Hundertmark, M.,
%A Johnson, J. A.,
%A Jrgensen, U. G.,
%A Kandori, R.,
%A Almeida, Leonardo Andrade,
%A Jablonski, F.,
%@affiliation IRAP, Université de Toulouse, CNRS, 14 Avenue Edouard Belin, 31400 Toulouse, France
%@affiliation Department of Physics, Chungbuk National University, Cheongju 361-763, Republic of Korea
%@affiliation Department of Physics, Chungbuk National University, Cheongju 361-763, Republic of Korea
%@affiliation IRAP, Université de Toulouse, CNRS, 14 Avenue Edouard Belin, 31400 Toulouse, France
%@affiliation Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA
%@affiliation South African Astronomical Observatory, P.O. Box 9, Observatory 7925, South Africa
%@affiliation UPMC-CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98bis boulevard Arago, F-75014 Paris, France
%@affiliation Department of Physics, 225 Nieuwland Science Hall, University of Notre Dame, Notre Dame, IN 46556, USA
%@affiliation Institute for Information and Mathematical Sciences, Massey University, Private Bag 102-904, Auckland 1330, New Zealand
%@affiliation Institute for Advanced Study, Einstein Drive, Princeton, NJ 08540, USA
%@affiliation Institute of Theoretical Physics, Charles University, V Holešovičkách 2, 18000 Prague, Czech Republic
%@affiliation UPMC-CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98bis boulevard Arago, F-75014 Paris, France
%@affiliation Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA
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%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
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%@electronicmailaddress leonardo@das.inpe.br
%B Astrophysical Journal
%V 754
%N 1
%P 73
%K gravitational lensing: micro, planetary systems.
%X 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.
%@language pt
%3 0004-637X_754_1_73.pdf