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We present an investigation into the kinematics of HD 106906 using the newlyreleased Gaia DR2 catalog to search for close encounters with other members ofthe Scorpius-Centaurus (Sco-Cen) association. HD 106906 is an eccentricspectroscopic binary that hosts both a large asymmetric debris disk extendingout to at least 500 au and a directly imaged planetary-mass companion at aprojected separation of 738 au. The cause of the asymmetry in the debris diskand the unusually wide separation of the planet is not currently known. Using acombination of Gaia DR2 astrometry and ground-based radial velocities, weexplore the hypothesis that a close encounter with another cluster memberwithin the last 15 Myr is responsible for the present configuration of thesystem. Out of 461 stars analyzed, we identified two candidate perturbers thathad a median closest approach (CA) distance within 1 pc of HD 106906: HIP 59716at $D_{\rm CA}=0.65_{-0.40}^{+0.93}$ pc ($t_{\rm CA}=-3.49_{-1.76}^{+0.90}$Myr) and HIP 59721 at $D_{\rm CA}=0.71_{-0.11}^{+0.18}$ pc ($t_{\rmCA}=-2.18_{-1.04}^{+0.54}$ Myr), with the two stars likely forming a widephysical binary. The trajectories of both stars relative to HD 106906 arealmost coplanar with the inner disk ($\Delta\theta = 5.4\pm1.7$ deg and$4.2_{-1.1}^{+0.9}$ deg). These two stars are the best candidates of thecurrently known members of Sco-Cen for having a dynamically important closeencounter with HD 106906, which may have stabilized the orbit of HD 106906 b inthe scenario where the planet formed in the inner system and attained higheccentricity by interaction with the central binary.

A Near-coplanar Stellar Flyby of the Planet Host Star HD 106906