posted on 2019-09-24, 16:31authored byDP Bennett, A Udalski, C Han, IA Bond, JP Beaulieu, J Skowron, BS Gaudi, N Koshimoto, F Abe, Y Asakura, RK Barry, A Bhattacharya, M Donachie, P Evans, A Fukui, Y Hirao, Y Itow, MCA Li, CH Ling, K Masuda, Y Matsubara, Y Muraki, M Nagakane, K Ohnishi, H Oyokawa, C Ranc, NJ Rattenbury, MM Rosenthal, T Saito, A Sharan, DJ Sullivan, T Sumi, D Suzuki, PJ Tristram, A Yonehara, MK Szymański, R Poleski, I Soszyński, K Ulaczyk, Wyrzykowski, D Depoy, A Gould, RW Pogge, JC Yee, MD Albrow, E Bachelet, V Batista, R Bowens-Rubin, S Brillant, JAR Caldwell, A Cole, C Coutures, S Dieters, DD Prester, J Donatowicz, P Fouqué, K Horne, M Hundertmark, N Kains, SR Kane, JB Marquette, J Menzies, KR Pollard, KC Sahu, J Wambsganss, A Williams, M Zub
We present the analysis of the microlensing event MOA-2010-BLG-117, and show that the light curve can only be explained by the gravitational lensing of a binary source star system by a star with a Jupiter-mass ratio planet. It was necessary to modify standard microlensing modeling methods to find the correct light curve solution for this binary source, binary-lens event. We are able to measure a strong microlensing parallax signal, which yields the masses of the host star, M∗= 0.58 ±0.11 Mo, and planet, mp= 0.54 ±0.10MJup, at a projected star-planet separation of a = 2.42 ±0.26 au, corresponding to a semimajor axis of a = 2.9-0.6+1.6au. Thus, the system resembles a half-scale model of the Sun-Jupiter system with a half-Jupiter0mass planet orbiting a half-solar-mass star at very roughly half of Jupiter's orbital distance from the Sun. The source stars are slightly evolved, and by requiring them to lie on the same isochrone, we can constrain the source to lie in the near side of the bulge at a distance of DS= 6.9 ±0.7 kpc, which implies a distance to the planetary lens system of DL= 3.5 ±0.4 kpc. The ability to model unusual planetary microlensing events, like this one, will be necessary to extract precise statistical information from the planned large exoplanet microlensing surveys, such as the WFIRST microlensing survey.
Funding
D.P.B., A.B., and D.S. were supported by NASA through grant NASA-NNX12AF54G. This work was partially supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The OGLE Team thanks Profs. M. Kubiak and G. Pietrzyński for their contribution to the collection of OGLE photometric data. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. The work by C.R. was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by USRA through a contract with NASA. The work by N.K. is supported by JSPS KAKENHI Grant Number JP15J01676. A.G. and B.S.G. were supported by NSF grant AST 110347 and by NASA grant NNX12AB99G.
History
Citation
Astronomical Journal, 2018, 155 (3)
Author affiliation
/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy