Notes. References^RX for the quoted values are provided as in Table G.1. Column 8 shows the disc extent.

¹M_P: Primary Mass: same as in Table C.1: estimated as described in Appendix C; Config.: Architecture of the system: lower case letters indicate planetary companions, capital letters indicate stellar or brown dwarf companions; Sep: semi-major axis for those companions with orbital constraints (Sep< 100 au) or separation for those on wider orbits (homogenised to angular units with parallaxes from Gaia DR3); M_c : Companion Mass: for substellar companions the units are given in Jupiter masses, while for stellar companions the mass is given in solar masses. If provided in the referenced literature, the uncertainties are given in ∆M_c ²Approximated disc extent. Values of R and ∆R are taken from Table B.1 ³HD 76582 and HD 76543 reported by Kervella et al. (2022) and Shaya & Olling (2011) as a common proper motion pair. In addition to the finding from Gaia Collaboration (2023), the two stars are at the same distance and have radial velocities that are consistent within the errors. No mass is reported for the companion; instead, a placeholder (‘?’) is used. This is because Kervella et al. (2022) does not provide a mass estimate, and the masses for both components reported in other studies, such as Shaya & Olling (2011) and De Rosa et al. (2014), are inconsistent with the primary star adopted here and with each other. ⁴ Hierarchical stellar triple system: The primary star HD 197481 (AU Mic) hosts two confirmed planets; and there are hints for two additional planets (Donati et al. 2023). It has a very wide companion HD 196982 (AT Mic), which is itself a binary system. Elliott et al. (2016) suggest a limit for wide binaries in the beta Pic moving group that agrees with HD 197481 (AU Mic) and HD 196982 (AT Mic) being bound in the past. However, the systems are considered comoving but not bound in Tokovinin (2018).