@Article{BacheletSHFGMBBBDHMMSSSUAAAABBBCCCCDDDGGHHHHJJKAJ:2012:COMAMI,
author = "Bachelet, E. and Shin, I. -G. and Han, C. and Fouqu{\'e}, P. and
Gould, A. and Menzies, J. W. and Beaulieu, J. -P. and Bennett, D.
P. and Bond, I. A. and Dong, Subo and Heyrovsk, D. and Marquette,
J. -B. and Marshall, J. and Skowron, J. and Street, R. A. and
Sumi, T. and Udalski, A. and Abe, L. and Agabi, K. and Albrow, M.
D. and Allen, W. and Bertin, E. and Bos, M. and Bramich, D. M. and
Chavez, J. and Christie, G. W. and Cole, A. A. and Crouzet, N. and
Dieters, S. and Dominik, M. and Drummond, J. and Greenhill, J. and
Guillot, T. and Henderson, C. B. and Hessman, F. V. and Horne, K.
and Hundertmark, M. and Johnson, J. A. and Jrgensen, U. G. and
Kandori, R. and Almeida, Leonardo Andrade and Jablonski, F.",
affiliation = "IRAP, Universit{\'e} de Toulouse, CNRS, 14 Avenue Edouard Belin,
31400 Toulouse, France and Department of Physics, Chungbuk
National University, Cheongju 361-763, Republic of Korea and
Department of Physics, Chungbuk National University, Cheongju
361-763, Republic of Korea and IRAP, Universit{\'e} de Toulouse,
CNRS, 14 Avenue Edouard Belin, 31400 Toulouse, France and
Department of Astronomy, Ohio State University, 140 West 18th
Avenue, Columbus, OH 43210, USA and South African Astronomical
Observatory, P.O. Box 9, Observatory 7925, South Africa and
UPMC-CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98bis
boulevard Arago, F-75014 Paris, France and Department of Physics,
225 Nieuwland Science Hall, University of Notre Dame, Notre Dame,
IN 46556, USA and Institute for Information and Mathematical
Sciences, Massey University, Private Bag 102-904, Auckland 1330,
New Zealand and Institute for Advanced Study, Einstein Drive,
Princeton, NJ 08540, USA and Institute of Theoretical Physics,
Charles University, V Holešovi\čk{\'a}ch 2, 18000 Prague,
Czech Republic and UPMC-CNRS, UMR 7095, Institut d'Astrophysique
de Paris, 98bis boulevard Arago, F-75014 Paris, France and
Department of Astronomy, Ohio State University, 140 West 18th
Avenue, Columbus, OH 43210, USA and {} and {} and {} and {} and {}
and {} and {} and {} and {} and {} and {} and {} and {} and {} and
{} and {} and {} and {} and {} and {} and {} and {} and {} and {}
and {} and {} and {} and {Instituto Nacional de Pesquisas
Espaciais (INPE)} and {Instituto Nacional de Pesquisas Espaciais
(INPE)}",
title = "MOA 2010-BLG-477Lb: CONSTRAINING THE MASS OF A MICROLENSING PLANET
FROM MICROLENSING PARALLAX, ORBITAL MOTION, AND DETECTION OF
BLENDED LIGHT",
journal = "Astrophysical Journal",
year = "2012",
volume = "754",
number = "1",
pages = "73",
month = "July",
keywords = "gravitational lensing: micro, planetary systems.",
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.",
doi = "10.1088/0004-637X/754/1/73",
url = "http://dx.doi.org/10.1088/0004-637X/754/1/73",
issn = "0004-637X and 1538-4357",
label = "lattes: 7812463045514059 41
BacheletSHFGMBBBDHMMSSSUAAAABBBCCCCDDDGGHHHHJJKA:2012:COMAMI",
language = "pt",
targetfile = "0004-637X_754_1_73.pdf",
urlaccessdate = "30 abr. 2024"
}