OGLE-2017-BLG-1049: Another giant planet microlensing event

We report a giant exoplanet discovery in the microlensing event OGLE-2017-BLG-1049, which is a planet-host star mass ratio of \(q=9.53\pm0.39\times10^{-3}\) and has a caustic crossing feature in the Korea Microlensing Telescope Network (KMTNet) observations. The caustic crossing feature yields an angular Einstein radius of \(\theta_{\rm E}=0.52 \pm 0.11\ {\rm mas}\). However, the microlens parallax is not measured because of the time scale of the event \(t_{\rm E}\simeq 29\ {\rm days}\), which is not long enough in this case to determine the microlens parallax. Thus, we perform a Bayesian analysis to estimate physical quantities of the lens system. From this, we find that the lens system has a star with mass \(M_{\rm h}=0.55^{+0.36}_{-0.29} \ M_{\odot}\) hosting a giant planet with \(M_{\rm p}=5.53^{+3.62}_{-2.87} \ M_{\rm Jup}\), at a distance of \(D_{\rm L}=5.67^{+1.11}_{-1.52}\ {\rm kpc}\). The projected star-planet separation in units of the Einstein radius \((\theta_{\rm E})\) corresponding to the total mass of the lens system is \(a_{\perp}=3.92^{+1.10}_{-1.32}\ \rm{au}\). This means that the planet is located beyond the snow line of the host. The relative lens-source proper motion is \(\mu_{\rm rel}\sim 7 \ \rm{mas \ yr^{-1}}\), thus the lens and source will be separated from each other within 10 years. Then the flux of the host star can be measured by a 30m class telescope with high-resolution imaging in the future, and thus its mass can be determined.