  The orbital distribution of giant planets is crucial for understanding how
terrestrial planets form and predicting yields of exoplanet surveys. Here, we
derive giant planets occurrence rates as a function of orbital period by taking
into account the detection efficiency of the Kepler and radial velocity (RV)
surveys. The giant planet occurrence rates for Kepler and RV show the same
rising trend with increasing distance from the star. We identify a break in the
RV giant planet distribution between ~2-3 au -- close to the location of the
snow line in the Solar System -- after which the occurrence rate decreases with
distance from the star. Extrapolating a broken power-law distribution to larger
semi-major axes, we find good agreement with the ~ 1% planet occurrence rates
from direct imaging surveys. Assuming a symmetric power law, we also estimate
that the occurrence of giant planets between 0.1-100 au is 26.6 +7.5 -5.4% for
planets with masses 0.1-20MJ and decreases to 6.2 +1.5 -1.2% for planets more
massive than Jupiter. This implies that only a fraction of the structures
detected in disks around young stars can be attributed to giant planets.
Various planet population synthesis models show good agreement with the
observed distribution, and we show how a quantitative comparison between model
and data can be used to constrain planet formation and migration mechanisms.
