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We report a giant exoplanet discovery in the microlensing eventOGLE-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 KoreaMicrolensing Telescope Network (KMTNet) observations. The caustic crossingfeature 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 timescale of the event $t_{\rm E}\simeq 29\ {\rm days}$, which is not long enoughin this case to determine the microlens parallax. Thus, we perform a Bayesiananalysis to estimate physical quantities of the lens system. From this, we findthat the lens system has a star with mass $M_{\rm h}=0.55^{+0.36}_{-0.29} \M_{\odot}$ hosting a giant planet with $M_{\rm p}=5.53^{+3.62}_{-2.87} \ M_{\rmJup}$, at a distance of $D_{\rm L}=5.67^{+1.11}_{-1.52}\ {\rm kpc}$. Theprojected star-planet separation in units of the Einstein radius $(\theta_{\rmE})$ 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 islocated beyond the snow line of the host. The relative lens-source propermotion is $\mu_{\rm rel}\sim 7 \ \rm{mas \ yr^{-1}}$, thus the lens and sourcewill be separated from each other within 10 years. Then the flux of the hoststar can be measured by a 30m class telescope with high-resolution imaging inthe future, and thus its mass can be determined.

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