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_Sun 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.
