We constrain the host-star flux of the microlensing planet OGLE-2014-BLG-0676Lb using adaptive optics (AO) images taken by the Magellan and Keck telescopes. We measure the flux of the light blended with the microlensed source to be K = 16.79 ± 0.04 mag and J = 17.76 ± 0.03 mag. Assuming that the blend is the lens star, we find that the host is a 0.73 − 0.29 + 0.14 M ⊙ star at a distance of 2.67 − 1.41 + 0.77 kpc, where the relatively large uncertainty in angular Einstein radius measurement is the major source of uncertainty. With mass of M p = 3.68 − 1.44 + 0.69 M J , the planet is likely a “super Jupiter” at a projected separation of r ⊥ = 4.53 − 2.50 + 1.49 AU, and a degenerate model yields a similar M p = 3.73 − 1.47 + 0.73 M J at a closer separation of r ⊥ = 2.56 − 1.41 + 0.84 AU. Our estimates are consistent with the previous Bayesian analysis based on a Galactic model. OGLE-2014-BLG-0676Lb belongs to a sample of planets discovered in a “second-generation” planetary microlensing survey and we attempt to systematically constrain host properties of this sample with high-resolution imaging to study the distribution of planets.
We present the discovery of a planet on a very wide orbit in the microlensing event OGLE-2012-BLG-0838. The signal of the planet is well separated from the main peak of the event and the planet-star projected separation is found to be twice larger than the Einstein ring radius, which roughly corresponds to a projected separation of ≈ 4 AU. Similar planets around low-mass stars are very hard to find using any technique other than microlensing. We discuss microlensing model fitting in detail and discuss the prospects for measuring the mass and distance of lens system directly.
We report adaptive-optics (AO) follow-up imaging of OGLE-2014-BLG-1050, which is the second binary microlensing event with space-based parallax measurements. The degeneracy in microlens parallax π E led to two sets of solutions, either a ∼ (0.9, 0.35) M binary at ∼ 3.5 kpc, or a ∼ (0.2, 0.07) M binary at ∼ 1.1 kpc. We measure the flux blended with the microlensed source by conducting Magellan AO observations, and find that the blending is consistent with the predicted lens flux from the higher-mass solution. From the combination of the AO flux measurement together with previous lensing constraints, it is estimated that the lens system consists of a 1.05 +0.08 −0.07 M primary and a 0.38 +0.07 −0.06 M secondary at 3.43 +0.19 −0.21 kpc.
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