line profiles [@Dent2005; @Pontoppidan2008; @Lyo2011] and of the stellar rotation [@Mueller2011] for SAO 206462 are consistent with an almost face-on geometry for the system ($i$$\sim$11$^{\circ}$). The star is actively accreting [$\sim$10$^{-11}$–10$^{-8}$ $M_{\odot}$/yr, @GarciaLopez2006; @Grady2009]. The disk is composed of a [massive outer component [up to $\sim$2$''$ i.e. $\sim$300 au, @Lyo2011] with masses for the dust $M_{\mathrm{dust}}$$=$1.3$\times$10$^{-4}$ $M_{\odot}$ and gas $M_{\mathrm{gas}}$$=$1.5$\times$10$^{-2}$ $M_{\odot}$ [@vanderMarel2016a]]{}, scattered-light spiral features [within $\sim$80 au]{} indicative of dynamical processes [@Muto2012], a large inner sub-mm dust cavity [[$\sim$50 au]{}, @Andrews2011], and a sub-au dust accretion disk [@Fedele2008; @Carmona2014; @Menu2015]. Recently, @Stolker2016 presented SPHERE optical and near-IR polarimetric images showing shadowing of the outer disk by warping/perturbation of the inner disk and the (marginal) detection of scattered light [up to $\sim$160 au]{}.

[One plausible explanation]{} for the spiral features seen in the SAO 206462 system is that they might be driven by planets. Two approaches have been used [to investigate]{} this hypothesis in the literature. The first approach consists in fitting analytical formulae derived for linear perturbations, i.e. one planet driving one spiral, to the observations. @Muto2012 proposed two planets located beyond $\sim$50 au with masses of $\sim$0.5 $M_{\rm{J}}$. Recently, @Stolker2016 used a similar approach assuming two planets located 