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We describe the SpHere INfrared Exoplanet (SHINE) survey, a key part of the SPHERE GTO Program on the ESO VLT, and present new statistical analyses of the frequency of gas giant planet occurrence as a function of host star mass. Constraining the frequency of the most massive planets, as well as the lowest mass brown dwarf companions, at wide orbital separations vs. host star mass, enables us to constrain key properties of exoplanet demographics such as the orbital surface density distribution and planet mass function, fundamental to a complete description of planetary architectures. In addition, our data provides a strong test of predictive theories of star and planet formation. This high contrast imaging survey has discovered and characterized dozens of very low mass companions (1-76 MJUPITER), on wide orbits (10-1000 AU) around a range of host star masses (0.3-3 MSUN). Our survey, constraining the frequency of gas giants, as well as brown dwarf companions, from 10-100 AU, suggests: 1) the frequency of gas giants around FGK (and other) stars peaks between 1-10 AU 2) the gas giant planet mass function appears to be a universal power-law relative to host star mass, explaining the trend of gas giant detection rate of with star mass 3) the brown dwarf companion mass function is consistent with extrapolation from a universal stellar companion mass ratio distribution down to the minimum mass for fragmentation

Michael Meyer: Frequency of Massive, Wide-orbit planets vs Stellar Mass: SPHERE shines on the ESO VLT