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A Likely Detection of a Two-planet System in a Low-magnification Microlensing Event
Suzuki, D.,Bennett, D. P.,Udalski, A.,Bond, I. A.,Sumi, T.,Han, C.,Kim, Ho-il.,Abe, F.,Asakura, Y.,Barry, R. K.,Bhattacharya, A.,Donachie, M.,Freeman, M.,Fukui, A.,Hirao, Y.,Itow, Y.,Koshimoto, N.,Li, American Astronomical Society 2018 The Astronomical journal Vol.155 No.6
The First Planetary Microlensing Event with Two Microlensed Source Stars
Bennett, D. P.,Udalski, A.,Han, C.,Bond, I. A.,Beaulieu, J.-P.,Skowron, J.,Gaudi, B. S.,Koshimoto, N.,Abe, F.,Asakura, Y.,Barry, R. K.,Bhattacharya, A.,Donachie, M.,Evans, P.,Fukui, A.,Hirao, Y.,Itow, American Astronomical Society 2018 The Astronomical journal Vol.155 No.3
A Planetary Microlensing Event with an Unusually Red Source Star: MOA-2011-BLG-291
Bennett, David P.,Udalski, Andrzej,Bond, Ian A.,Suzuki, Daisuke,Ryu, Yoon-Hyun,Abe, Fumio,Barry, Richard K.,Bhattacharya, Aparna,Donachie, Martin,Fukui, Akihiko,Hirao, Yuki,Kawasaki, Kohei,Kondo, Iona American Astronomical Society 2018 The Astronomical journal Vol.156 No.3
OGLE-2017-BLG-0482Lb: A Microlensing Super-Earth Orbiting a Low-mass Host Star
Han, C.,Hirao, Y.,Udalski, A.,Lee, C.-U.,Bozza, V.,Gould, A.,Abe, F.,Barry, R.,Bond, I. A.,Bennett, D. P.,Bhattacharya, A.,Donachie, M.,Evans, P.,Fukui, A.,Itow, Y.,Kawasaki, K.,Koshimoto, N.,Li, M. C American Astronomical Society 2018 The Astronomical journal Vol.155 No.5
Ground-based Parallax Confirmed by<i>Spitzer</i>: Binary Microlensing Event MOA-2015-BLG-020
Wang, Tianshu,Zhu, Wei,Mao, Shude,Bond, I. A.,Gould, A.,Udalski, A.,Sumi, T.,Bozza, V.,Ranc, C.,Cassan, A.,Yee, J. C.,Han, C.,Abe, F.,Asakura, Y.,Barry, R.,Bennett, D. P.,Bhattacharya, A.,Donachie, M. American Astronomical Society 2017 The Astrophysical journal Vol.845 No.2
<P>We present the analysis of the binary gravitational microlensing event MOA-2015-BLG-020. The event has a fairly long timescale (similar to 63 days) and thus the light curve deviates significantly from the lensing model that is based on the rectilinear lens-source relative motion. This enables us to measure the microlensing parallax through the annual parallax effect. The microlensing parallax parameters constrained by the ground-based data are confirmed by the Spitzer observations through the satellite parallax method. By additionally measuring the angular Einstein radius from the analysis of the resolved caustic crossing, the physical parameters of the lens are determined. It is found that the binary lens is composed of two dwarf stars with masses M-1= 0.606 +/- 0.028M(circle dot) and M-2= 0.125 +/- 0.006 M-circle dot in the Galactic disk. Assuming that the source star is at the same distance as the bulge red clump stars, we find the lens is at a distance D-L = 2.44 +/- 0.10 kpc. We also provide a summary and short discussion of all of the published microlensing events in which the annual parallax effect is confirmed by other independent observations.</P>