Journal article
MOA-2009-BLG-387Lb: a massive planet orbiting an M dwarf
Astronomy & Astrophysics, Vol.529
May/2011
Abstract
Aims. We report the discovery of a planet with a high planet-to-star mass ratio in the microlensing event MOA-2009-BLG-387, which exhibited pronounced deviations over a 12-day interval, one of the longest for any planetary event. The host is an M dwarf, with a mass in the range 0.07 M-circle dot <M-host <0.49 M-circle dot at 90% confidence. The planet-star mass ratio q = 0.0132 +/- 0.003 has been measured extremely well, so at the best-estimated host mass, the planet mass is m(p) = 2.6 Jupiter masses for the median host mass, M = 0.19 M-circle dot. Methods. The host mass is determined from two "higher order" microlensing parameters. One of these, the angular Einstein radius theta(E) = 0.31 +/- 0.03 mas has been accurately measured, but the other (the microlens parallax pi(E), which is due to the Earth's orbital motion) is highly degenerate with the orbital motion of the planet. We statistically resolve the degeneracy between Earth and planet orbital effects by imposing priors from a Galactic model that specifies the positions and velocities of lenses and sources and a Kepler model of orbits. Results. The 90% confidence intervals for the distance, semi-major axis, and period of the planet are 3.5 kpc <D-L <7.9 kpc, 1.1 AU <a <2.7 AU, and 3.8 yr <P <7.6 yr, respectively.
Details
- Title
- MOA-2009-BLG-387Lb; a massive planet orbiting an M dwarf
- Creators
- V. Batista (null)A. Gould (null)S. Dieters (null)S. Dong (null)I. Bond (null)J. P. Beaulieu (null)D. Maoz (null)B. Monard (null)G. W. Christie (null)J. McCormick (null)M. D. Albrow (null)K. Horne (null)Y. Tsapras (null)M. J. Burgdorf (null)S. Calchi Novati (null)J. Skottfelt (null)J. Caldwell (null)S. Kozlowski (null)D. Kubas (null)
- Resource Type
- Journal article
- Publication Details
- Astronomy & Astrophysics, Vol.529; May/2011
- Number of pages
- 16
- Language
- English
- DOI
- https://doi.org/10.1051/0004-6361/201016111
- Grant note
- HOLMES [ANR-06-BLAN-0416]; NSF [AST-0757888, AST-0206189, AST-0708890]; NASA [NNG04GL51G, NAF5-13042, NNX07AL71G]; Polish MNiSW [N20303032/4275, HST-GO-11311]; Korea Science and Engineering Foundation [2009-008561]; Korea Research Foundation [2006-311-C00072]; Korea Astronomy and Space Science Institute (KASI); Deutsche Forschungsgemeinschaft; PPARC/STFC; EU; Dill Faulkes Educational Trust (Faulkes Telescope North); Marsden Fund of NZ; Foundation for Research Science and Technology of NZ; Creative Research Initiative program [2009-008561]; Chinese Academy of Sciences (CAS) [2009Y2AJ7]; [JSPS18253002]; [JSPS20340052]; [JSPS19340058]; [MEXT19015005]; [JSPS18749004]V.B. thanks Ohio State University for its hospitality during a six week visit, during which this study was initiated. We acknowledge the following support: Grants HOLMES ANR-06-BLAN-0416 Dave Warren for the Mt Canopus Observatory; NSF AST-0757888 (AG, SD); NASA NNG04GL51G (DD, AG, RP); Polish MNiSW N20303032/4275 (AU); HST-GO-11311 (KS); NSF AST-0206189 and AST-0708890, NASA NAF5-13042 and NNX07AL71G (DPB); Korea Science and Engineering Foundation grant 2009-008561 (CH); Korea Research Foundation grant 2006-311-C00072 (B-GP); Korea Astronomy and Space Science Institute (KASI); Deutsche Forschungsgemeinschaft (CSB); PPARC/STFC, EU FP6 programme "ANGLES" (LW, NJR); PPARC/STFC (RoboNet); Dill Faulkes Educational Trust (Faulkes Telescope North); Grants JSPS18253002, JSPS20340052 and JSPS19340058 (MOA); Marsden Fund of NZ(IAB, PCMY); Foundation for Research Science and Technology of NZ; Creative Research Initiative program (2009-008561) (CH); Grants MEXT19015005 and JSPS18749004 (TS). Work by S. D. was performed under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. J.C.Y. is supported by an NSF Graduate Research Fellowship. This work was supported in part by an allocation of computing time from the Ohio Supercomputer Center. J.A. is su_ALMAME_DELIMITER_
- Scientific Unit
- The Weizmann Institute of Science
- Record Identifier
- 993264289203596
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