www.postersession.com www.postersession.com Stars are thought to be commonly born and found in binary/ multiple systems. The diverse orbital configurations and rich dynamics in planet-bearing binary systems provide valuable conditions to test various theories and models of planet formation and evolution Conclusions We build our planet sample by retrieving data (on 04-March- 2021) from two online catalogues. i.e., (1) the catalog of exoplanet-hosting binaries with separations up to 500 AU[1], (2) the catalogue of exoplanets in binary star systems [2]. Furthermore, in order to have a unified criteria to define our sample, we adopted an upper mass limit (20 mJ) for planetary objects and a lower mass limit (50 mJ) for stellar objects. Finally, we obtain 110 planets in 80 systems, 61 (19) of which are single (multiple) planet systems. Introduction *To whom corresponding maybe addressed. Email: jwxie@nju.edu.cn Demographics of Exoplanets in Binaries (DEB). I. Architecture of S-Type Planetary Systems Revealed by the RV Sample Xiang-Ning Su1,2，Ji-Wei Xie1,2*，Ji-Lin Zhou1,2，Philippe Thebault3 1 School of Astronomy and Space Science, Nanjing University, Nanjing 210023, People’s Republic of China 2 Key Laboratory of Modern Astronomy and Astrophysics, Ministry of Education, Nanjing 210023, People’s Republic of China 3 LESIA, Observatoire de Paris, Meudon Principal Cedex, France orbital configurations of planets in binaries Most planets in binaries are currently found in S-type, there are 211confirmed S-type planets. Among them, 116 are from radial velocity (RV) surveys, 89 from transit surveys and 6 from others. S-type: planets orbit one of the binary stars; P-type: planets orbit both the binary stars. sample heterogeneity and observational bias The sample heterogeneity and observational bias are obstacles toward a clear figure of exoplanet demographics in the binary environment. We only focus on S-type planet systems from RV surveys to reduce the sample complexity and thus better take into potential observational bias. Sample and Method Results quantifying the RV detection constraints We adopt RV signal injection-recovery test to quantify observational bias: • we collect the RV data of each system and extract the RV residual. • we inject a test RV signale, and generate a set of simulated RV data • we evaluate whether the injected planet signal can be recovered from the simulated RV data. single planets VS. multiple planets Multiple-planet systems are more prevalent in wide binaries whereas single-planet ones are, on average, found in tighter binaries. There are no difference between single and multiple planet systems in the statistics of planetary mass and eccentricity distributions after considering the effect of detection limit. But singles and multiples seem to differ significantly in the 2-D distribution of the period-mass diagram. There is a rectangular- shaped gap (period = 10-300 days and Msini = 160-640 )in the period-mass diagram of single-planet systems but not for multiples. Close VS. Wide Binaries The period-mass gap identified for single-planet systems is also preferentially found in close-binaries. There is a rising upper envelope planets in the period-mass diagram for wide binaries (and single star systems) which is not found in the close-binary subsample. 1. Single (multiple) planetary systems are mostly found in close (wide) binaries with separation aB< (>) 100- 300 AU. 2. In binaries, single and multiple-planet systems are similar in 1-D distributions of mass and period as well as eccentricity (in contrast to the "eccentricity dichotomy" found in single-star systems) but different in the 2-D period-mass diagram. Specifically, there is a rectangular-shaped gap in the period-mass diagram of single-planet systems but not for multiples. This gap also depends on binary separation and is more prominent in close binaries. 3. There is a rising upper envelope in the period-mass diagram for planets in wide binaries as well as in