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Masses and orbital constraints for the OGLE-2006-BLG-109Lb,c Jupiter/Saturn analog Planetary System


Bennett, DP and Rhie, SH and Nikolaev, S and Gaudi, BS and Udalski, A and Gould, A and Christie, GW and Maoz, D and Dong, S and McCormick, J and Szymanski, MK and Tristram, PJ and Macintosh, B and Cook, KH and Kubiak, M and Pietrzynski, G and Soszynski, I and Szewczyk, O and Ulaczyk, K and Wyrzykowski, L and DePoy, DL and Han, C and Kaspi, S and Lee, CU and Mallia, F and Natusch, T and Park, BG and Pogge, RW and Polishook, D and Abe, F and Bond, IA and Botzler, CS and Fukui, A and Hearnshaw, JB and Itow, Y and Kamiya, K and Korpela, AV and Kilmartin, PM and Lin, W and Ling, J and Masuda, K and Matsubara, Y and Motomura, M and Muraki, Y and Nakamura, S and Okumura, T and Ohnishi, K and Perrott, YC and Rattenbury, NJ and Sako, T and Saito, T and Sato, S and Skuljan, L and Sullivan, DJ and Sumi, T and Sweatman, WL and Yock, PCM and Albrow, M and Allan, A and Beaulieu, J-P and Bramich, DM and Burgdorf, MJ and Coutures, C and Dominik, M and Dieters, S and Fouque, P and Greenhill, J and Horne, K and Snodgrass, C and Steele, I and Tsapras, Y and Chaboyer, B and Crocker, A and Frank, S and the OGLE Collaboration, the μFUN Collaboration, the MOA Collaboration, and the PLANET and RoboNet Collaborations, Masses and orbital constraints for the OGLE-2006-BLG-109Lb,c Jupiter/Saturn analog Planetary System, Astrophysical Journal , 713, (2) pp. 837-855. ISSN 0004-637X (2010) [Refereed Article]

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Copyright 2010. The American Astronomical Society

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DOI: doi:10.1088/0004-637X/713/2/837


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 +0.05 -0.04 Mo, Mb = 231 19 M , and Mc = 86 7 M . 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 E=0.15 =+0.17 -0.10 and an orbital inclination of I=64o +4o -7o. The 95% confidence level lower limit on the inclination of i > 49 implies that this planetary system can be detected and studied via radial velocity measurements using a telescope of>~ 30 m aperture.

Item Details

Item Type:Refereed Article
Keywords:gravitational lensing: micro; planetary systems
Research Division:Physical Sciences
Research Group:Astronomical sciences
Research Field:Galactic astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding knowledge
Objective Field:Expanding knowledge in the physical sciences
UTAS Author:Beaulieu, J-P (Dr Jean-Philippe Beaulieu)
UTAS Author:Greenhill, J (Dr John Greenhill)
ID Code:63617
Year Published:2010
Web of Science® Times Cited:107
Deposited By:Physics
Deposited On:2010-05-18
Last Modified:2022-06-03
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