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The orbital distribution of giant planets is crucial for understanding howterrestrial planets form and predicting yields of exoplanet surveys. Here, wederive giant planets occurrence rates as a function of orbital period by takinginto account the detection efficiency of the Kepler and radial velocity (RV)surveys. The giant planet occurrence rates for Kepler and RV show the samerising trend with increasing distance from the star. We identify a break in theRV giant planet distribution between ~2-3 au -- close to the location of thesnow line in the Solar System -- after which the occurrence rate decreases withdistance from the star. Extrapolating a broken power-law distribution to largersemi-major axes, we find good agreement with the ~ 1% planet occurrence ratesfrom direct imaging surveys. Assuming a symmetric power law, we also estimatethat the occurrence of giant planets between 0.1-100 au is 26.6 +7.5 -5.4% forplanets with masses 0.1-20MJ and decreases to 6.2 +1.5 -1.2% for planets moremassive than Jupiter. This implies that only a fraction of the structuresdetected in disks around young stars can be attributed to giant planets.Various planet population synthesis models show good agreement with theobserved distribution, and we show how a quantitative comparison between modeland data can be used to constrain planet formation and migration mechanisms.

Hints for a Turnover at the Snow Line in the Giant Planet Occurrence Rate