Notes. M_⋆ is the mass of the primary star in the system; $a_{\text{cav}}^{\text{obs}}$ is the semi-major axis of the gas cavity, obtained using $a_{\text{cav}}^{\text{obs}}$ = 0.75 × R_mm, with R_mm the location of the dust cavity ring, as reported by van der Marel et al. (2021); $q_{\mathrm{s}\mathrm{p}}^{\pm }$ and $q_{\mathrm{c}\mathrm{o}\mathrm{r}}^{\pm }$ are conservative and optimistic companion mass-ratio detection limits (Eqs. (8) and (9)) from sparse aperture masking and from coronagraph studies, respectively, based on the minimum and maximum values in the detection curves in van der Marel et al. (2021); and R_sp, and R_cor are sparse aperture masking and coronagraph reference radii (see Eqs. (8) and (9)). ${\mathcal{L}}_{\text{bin}}^{\pm }$ and ${\mathcal{L}}_{\text{pl}}^{\pm }$ are conservative and optimistic cumulative probabilities at the cavity edge (P[d < R = a_cav]) for binaries and planets, respectively. These quantities represent the total likelihood that a companion remains undetected within the cavity under the hypothesis a companion carves it. ⁽¹⁾The detection limits for HD 142527 are for a tertiary undetected companion that carves the cavity. The detected binary in the system is too compact to carve the a_cav = 135 au cavity (Nowak et al. 2024); $q_{\mathrm{s}\mathrm{p}}^{\pm }=0$ up to R_sp = 30 are placed to account for orbital stability considerations around the binary in the system. ⁽²⁾For AB Aur, detection limits on the Pa β planet accretion tracer are available (Biddle et al. 2024; Currie 2024), but were not converted into upper mass limits. ⁽³⁾For HD 135344B, the newer upper limits presented by Stolker et al. (2024) appear to be less conservative (higher upper limits) at large radii than those adopted by van der Marel et al. (2021). We retained the more conservative values from van der Marel et al. (2021).