期刊
ASTROPHYSICAL JOURNAL
卷 713, 期 2, 页码 837-855出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/713/2/837
关键词
gravitational lensing: micro; planetary systems
资金
- NSF [AST-0708890, AST-0757888]
- NASA [NNX07AL71G, NNG04GL51G]
- Polish MNiSW [N20303032/4275]
- U.S. Department of Energy [DE-AC52-07NA27344]
- JSPS [JSPS18749004]
- National Research Fund of Korea [2009-0081561]
- Korea Astronomy and Space Science Institute
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0757888] Funding Source: National Science Foundation
- Science and Technology Facilities Council [ST/G001987/1, ST/G009465/1, PP/E001149/1, PP/E002137/1, ST/H002391/1] Funding Source: researchfish
- STFC [ST/G009465/1, ST/H002391/1, PP/E001149/1, ST/G001987/1, PP/E002137/1] Funding Source: UKRI
We present a new analysis of the Jupiter+Saturn analog system, OGLE-2006-BLG-109Lb,c, which was the first double planet system discovered with the gravitational microlensing method. This is the only multi-planet system discovered by any method with measured masses for the star and both planets. In addition to the signatures of two planets, this event also exhibits a microlensing parallax signature and finite source effects that provide a direct measure of the masses of the star and planets, and the expected brightness of the host star is confirmed by Keck AO imaging, yielding masses of M-* = 0.51(-0.04)(+0.05) M-circle dot, M-b = 231 +/- 19 M-circle plus, and M-c = 86 +/- 7 M-circle plus. The Saturn-analog planet in this system had a planetary light-curve deviation that lasted for 11 days, and as a result, the effects of the orbital motion are visible in the microlensing light curve. We find that four of the six orbital parameters are tightly constrained and that a fifth parameter, the orbital acceleration, is weakly constrained. No orbital information is available for the Jupiter-analog planet, but its presence helps to constrain the orbital motion of the Saturn-analog planet. Assuming co-planar orbits, we find an orbital eccentricity of epsilon = 0.15(-0.10) (+0.17) and an orbital inclination of i = 64 degrees(+ 4 degrees)(-7 degrees) The 95% confidence level lower limit on the inclination of i > 49 degrees implies that this planetary system can be detected and studied via radial velocity measurements using a telescope of greater than or similar to 30 m aperture.
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