5σ detection limits in contrast with respect to the star (left) and in planet mass (right). For the conversion of the SPHERE contrast limits, we used the atmospheric and evolutionary models of Baraffe et al. (2015, and 2003), while for the NaCo contrast limits, we assumed the models of Allard et al. (2012) and Baraffe et al. (2003). The locations of the outer edge of the scattered-light cavity and the outer visibility radius of the spiral arms are also shown (Stolker et al. 2016). Greyed areas indicate theoretical planet predictions from Fung & Dong (2015) and Bae et al. (2016).