Notes. When both disks are detected, separations are measured as the distance between the fitted center of the two disks. Otherwise, the value is taken from the literature (White & Ghez 2001; Kraus & Hillenbrand 2009; Köhler et al. 2016). Distances are obtained by inverting the Gaia parallax when the uncertainty on the parallax is less than 10% of the measured parallax. See Sect. 2.1 for more information. The values q and μ are derived as described in Sect. 2.1. The last column reports whether ¹³ CO emission is detected. A question mark flags when the detection is contaminated by cloud emission. For the two triple systems (T Tau, UZ Tau), the first line reports the information for the primary and the center of mass of the secondary, while the second line reports the information on the secondary and tertiary stars. ^(†) The disk aroundthe primary component is a well-resolved transition disk (e.g., Long et al. 2018). ^(*) The disk around component A (north) is detected (see Appendix A.3).