the cavity [at a separation of 17.5–20 au]{} could be responsible for the different cavity sizes measured for the small and large dust grains. @Fung2015 presented scaling relations between the azimuthal separation of the primary and secondary arms and the planet-to-star mass ratio for a single companion on a circular orbit with a mass between Neptune mass and 16 $M_{\rm{J}}$ around a 1 $M_{\odot}$ star. They predicted [with 30% accuracy that a single putative planet responsible for both spiral features of SAO 206462 would have a mass of $\sim$6 $M_{\rm{J}}$]{}. @Bae2016 presented dedicated hydrodynamical simulations of the SAO 206462 disk and proposed that both the bright scattered-light feature [@Garufi2013] and the dust emission peak [@Perez2014] seen for the southwestern spiral arm result from the interaction of the spiral arm with a vortex, although a vortex alone can account for the [S1 brightness peak]{}. They suggested that a 10–15 $M_{\rm{J}}$ planet may orbit at 100–120 au from the star. However, ALMA observations at two different frequencies seem to contradict a dust particle trapping scenario by a vortex [@Pinilla2015]. @Stolker2016 performed new fitting of the spiral arms observed in SPHERE data and found a best-fit solution with two protoplanets located exterior to 