Light curve follow up of MOA-2020-BLG-208L

With a mass ratio q=3.17_-0.26_^+0.28^e-4, the planet lies near the peak of the mass-ratio function derived by the MOA collaboration and near the edge of expected sample sensitivity. For these estimates we provide results using two mass-law priors: one assuming that all stars have an equal planet-hosting probability, and the other assuming that planets are more likely to orbit around more massive stars.

In the first scenario, we estimate that the lens system is likely to be a planet of mass M_p_=46_-24_^+42^M{Earth} and a host star of mass M_s_=0.43_-0.23_^+0.39^M{sun}, located at a distance D_L_=7.49_-1.13_^+0.99^kpc. For the second scenario, we estimate M_p_=69_-34_^+37^M{Earth}, M_s_=0.66_-0.32_^+0.35^M{sun}, and D_L_=7.81_-0.93_^+0.93^kpc. The planet has a projected separation as a fraction of the Einstein ring radius s=1.3807_-0.0018_}^+0.0018^.