could still be low-mass planets in the outer disk and/or planets inside the cavity.]{}

Introduction
============

SAO206462 (HD135344B) is a rapidly rotating ($v$ sin $i$ $\sim$ 83 kms$^{-1}$) Herbig Ae/Be F4Ve star of age 9$\pm$2 Myr and mass 1.7$^{+0.2}_{-0.1}$ $M_{\odot}$ [@Mueller2011] [located at 156$\pm$11 pc [@GaiaCollaboration2016]]{} in the Upper Centaurus Lupus star-forming region, known to harbor a transitional disk resolved in scattered light [@Grady2009; @Muto2012; @Garufi2013; @Wahhaj2015; @Stolker2016] [and]{} in thermal emission, both at mid-IR [@Doucet2006; @Maaskant2013] and (sub-)mm wavelengths [@Brown2009; @Andrews2011; @Lyo2011; @Perez2014; @Pinilla2015; @vanderMarel2016a; @vanderMarel2016b]. It is part of a [widely separated ($\sim$21$''$, i.e. $\sim$3300 au) binary]{} with SAO 206463 [@Coulson1995]. Transitional disks are associated with an intermediate stage of disk evolution, where the dust opacity has been reduced (perhaps tracing [a]{} dip in the gas surface density) in the near- and mid-IR [e.g., @Strom1989; @Espaillat2014]. [Several scenarios have been proposed [that can explain]{} the gas and dust depletion [such as]{} photoevaporation, dust grain growth, [or ongoing]{} planet formation [@Hollenbach1994; @Dullemond2005; @Lin1993]]{}.

  UT date       Seeing ($''$)   $\tau_0$ (ms)   AM start/end      Mode          Bands       DIT(s)$\times$Nfr   $\Delta$PA ($^{\circ}$)      SR
  ------------ --------------- --------------- -------------- ------------- -------------- ------------------- ------------------------- -----------
  2015/05/15      0.45–0.57         7–10         1.04–1.03     IRDIFS\_EXT   $YJH$+$K1K2$     64$\times$64               63.6             0.78–0.85

Measurements of the CO 