Close binaries suppress the formation of circumstellar ( S-type ) planets and therefore significantly bias the inferred planet occurrence rates and statistical trends .
After compiling various radial velocity and high-resolution imaging surveys , we determine that binaries with a \lesssim 1 au fully suppress S-type planets , binaries with a \approx 10 au host close planets at \approx 15 % the occurrence rate of single stars , and wide binaries with a \gtrsim 200 au have a negligible effect on planet formation .
We show that F = 43 % \pm 6 % of solar-type primaries do not host close planets due to suppression by close stellar companions .
By removing spectroscopic binaries from their samples , radial velocity surveys for giant planets boost their detection rates by a factor of 1/ ( 1- F ) = 1.8 \pm 0.2 compared to transiting surveys .
This selection bias fully accounts for the discrepancy in hot Jupiter occurrence rates inferred from these two detection methods .
Correcting for both planet suppression by close binaries and transit dilution by wide binaries , the occurrence rate of small planets orbiting single G-dwarfs is 2.1 \pm 0.3 times larger than the rate inferred from all G-dwarfs in the Kepler survey .
About half ( but not all ) of the observed increase in small , short-period planets toward low-mass hosts can be explained by the corresponding decrease in the binary fraction .
Finally , we demonstrate that the apparent enhancement of wide stellar companions to hot Jupiter hosts is due to multiple selection effects .
Although very close binaries with secondary masses M _ { 2 } \gtrsim 10 M _ { J } preferentially have wide tertiary companions , genuine hot Jupiters with M _ { p } \approx 0.2 - 4 M _ { J } that formed via core accretion do not exhibit a statistically significant excess of wide stellar companions .