OGLE-2018-BLG-0567Lb and OGLE-2018-BLG-0962Lb: Two Microlensing Planets
  through Planetary-Caustic Channel
  We present the analyses of two microlensing events, OGLE-2018-BLG-0567 and
OGLE-2018-BLG-0962. In both events, the short-lasting anomalies were densely
and continuously covered by two high-cadence surveys. The light-curve modeling
indicates that the anomalies are generated by source crossings over the
planetary caustics induced by planetary companions to the hosts. The estimated
planet/host separation (scaled to the angular Einstein radius $\theta_{\rm E}$)
and mass ratio are $(s, q) = (1.81, 1.24\times10^{-3})$ and $(s, q) = (1.25,
2.38\times10^{-3})$, respectively. From Bayesian analyses, we estimate the host
and planet masses as $(M_{\rm h}, M_{\rm p}) =
(0.24_{-0.13}^{+0.16}\,M_{\odot}, 0.32_{-0.16}^{+0.34}\,M_{\rm J})$ and
$(M_{\rm h}, M_{\rm p}) = (0.55_{-0.29}^{+0.32}\,M_{\odot},
1.37_{-0.72}^{+0.80}\,M_{\rm J})$, respectively. These planetary systems are
located at a distance of $7.07_{-1.15}^{+0.93}\,{\rm kpc}$ for
OGLE-2018-BLG-0567 and $6.47_{-1.73}^{+1.04}\,{\rm kpc}$ for
OGLE-2018-BLG-0962, suggesting that they are likely to be near the Galactic
bulge. The two events prove the capability of current high-cadence surveys for
finding planets through the planetary-caustic channel. We find that most
published planetary-caustic planets are found in Hollywood events in which the
source size strongly contributes to the anomaly cross section relative to the
size of the caustic.
