Bennett, DP and Udalski, A and Han, C and Bond, IA and Beaulieu, J-P and Skowron, J and Gaudi, BS and Koshimoto, N and Abe, F and Asakura, Y and Barry, RK and Bhattacharya, A and Donachie, M and Evans, P and Fukui, A and Hirao, Y and Itow, Y and Li, MCA and Ling, CH and Masuda, K and Matsubara, Y and Muraki, Y and Nagakane, M and Ohnishi, K and Oyokawa, H and Ranc, C and Rattenbury, NJ and Rosenthal, MM and Saito, T and Sharan, A and Sullivan, DJ and Sumi, T and Suzuki, D and Tristram, PJ and Yonehara, A and Szymanski, MK and Poleski, R and Soszynski, I and Ulaczyk, K and Wyrzykowski, K and Depoy, D and Gould, A and Pogge, RW and Yee, JC and Albrow, MD and Bachelet, E and Batista, V and Bowens-Rubin, R and Brillant, S and Caldwell, JAR and Cole, A and Coutures, C and Dieters, S and Prester, DD and Donatowicz, J and Fouque, P and Horne, K and Hundertmark, M and Kains, N and Kane, SR and Marquette, JB and Menzies, J and Pollard, KR and Ranc, C and Sahu, KC and Wambsganss, J and Williams, A and Zub, M, The first planetary microlensing event with two microlensed source stars, Astronomical Journal, 155, (3) Article 141. ISSN 0004-6256 (2018) [Refereed Article]
© 2018. The American Astronomical Society. All rights reserved.
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 M ⊙, and planet, m p = 0.54 ± 0.10M Jup, at a projected star–planet separation of a ⊥ = 2.42 ± 0.26 au, corresponding to a semimajor axis of au. 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 D S = 6.9 ± 0.7 kpc, which implies a distance to the planetary lens system of D L = 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.
|Item Type:||Refereed Article|
|Keywords:||exoplanets, binary stars, planetary systems, microlensing|
|Research Division:||Physical Sciences|
|Research Group:||Astronomical and Space Sciences|
|Research Field:||Stellar Astronomy and Planetary Systems|
|Objective Division:||Expanding Knowledge|
|Objective Group:||Expanding Knowledge|
|Objective Field:||Expanding Knowledge in the Physical Sciences|
|UTAS Author:||Cole, A (Associate Professor Andrew Cole)|
|Web of Science® Times Cited:||3|
|Deposited By:||Mathematics and Physics|
|Downloads:||30 View Download Statistics|
Repository Staff Only: item control page