Characterizing microlensing planetary system OGLE-2014-BLG-0676Lb with adaptive optics imaging

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 ${0.73}_{-0.29}^{+0.14}{M}_{\odot }$ 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 ${r}_{\perp }={4.53}_{-2.50}^{+1.49}$ AU, and a degenerate model yields a similar ${M}_{p}={3.73}_{-1.47}^{+0.73}{M}_{J}$ at a closer separation of ${r}_{\perp }={2.56}_{-1.41}^{+0.84}$ 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. *This paper includes data gathered with the 6.5m Magellan Clay Telescope at Las Campanas Observatory, Chile.