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Although the sample of exoplanets in binaries has been greatly expanded, thesample heterogeneity and observational bias are obstacles toward a clear figureof exoplanet demographics in the binary environment. To overcome the obstacles,we conduct a statistical study that focuses on S-type planetary systemsdetected by the Radial Velocity method. We try to account for observationalbiases by estimating, from available RV data, planet detection efficiencies foreach individual system. Our main results are as follows: (1) Single (multiple)planetary systems are mostly found in close (wide) binaries with separationaB<(>)100-300 AU. (2) In binaries, single and multiple-planet systems aresimilar in 1-D distributions of mass and period as well as eccentricity (incontrast to the "eccentricity dichotomy" found in single-star systems) butdifferent in the 2-D period-mass diagram. Specifically, there is arectangular-shaped gap in the period-mass diagram of single-planet systems butnot for multiples. This gap also depends on binary separation and is moreprominent in close binaries. (3) There is a rising upper envelope in theperiod-mass diagram for planets in wide binaries as well as in single stars butnot in close binaries. More specifically, there is a population of massiveshort period planets in close binaries but almost absent in wide binaries orsingle stars. We suggest that enhanced planetary migration, collision, and /orejection in close binaries could be the potential underlying explanation forthese three features.

Demographics of Exoplanets in Binaries (DEB). I. Architecture of S-Type Planetary Systems Revealed by the RV Sample