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.
