density filter (transmission $\sim$1.78%) for a total integration time of 480s. No point source was detected close to the star. We computed the TLOCI 5$\sigma$ detection limits using the same parameters as in Sect. \[sec:datareduc\] [and corrected them for the small sample statistics [@Mawet2014].]{}

[The SPHERE and NaCo]{} contrast limits are shown in the left panel of Fig. \[fig:detlimits\]. The thermal background increases with the wavelength, hence the poorer contrast performance observed for IRDIS in the $K2$ band and NaCo in the $L^{\prime}$ band at large separations. The SPHERE contrasts are deeper than the NaCo contrasts by factors [greater]{} than $\sim$10 in the speckle-limited regions ($\lesssim$0.6$''$), illustrating the improved performances of new dedicated high-contrast instruments like SPHERE and GPI.

Comparison of the detection limits to planet predictions
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Several predictions for planet(s) shaping the disk of SAO 206462 have been proposed [@Muto2012; @Garufi2013; @Fung2015; @Bae2016; @vanderMarel2016b]. Using linear equations from the spiral density wave theory, @Muto2012 suggested two planets with separations beyond $\sim$50 au by fitting independently the two spiral arms seen in Subaru/HiCIAO data and with masses of $\sim$0.5 $M_{\rm{J}}$ by using the amplitude of the spiral wave. @Garufi2013 proposed that one planet of mass [5–13 $M_{\rm{J}}$]{} located inside 