Notes. References^RX for the quoted techniques as in Table G.1. Flags: ? = no data available and/or no conclusion on the (non)presence of a companion. Y = existing surveys report detected (gravitationally bound) stellar and/or substellar companions. Y? = RUWE and/or PMa and/or χ² and/or searches for CPM candidates indicate possible companions. N = existing surveys probing this separation range report non-detections → with (high) probability there are no companions. N? = values exist of PMa and/or RUWE that do not show signs of multiplicity Techniques: RV = Radial Velocity; AO = Adaptive Optics; PMa = Proper Motion Anomaly (mostly between HIPPARCOS and Gaia); RUWE = Renormalized Unit Weight Error (from Gaia); CPM = Common Proper Motion; T = Transit. Flags with the reference ^‘RTW’ correspond to contrast limits obtained homogeneously with the data available in the SPHERE data centre, stellar properties from Table 1, and the predictions in mass from the Baraffe et al. (2015) model using broad-band H filter (and if not available H_D2 and H_D3 filter) observations: we separated the outcomes into three regimes: RTW1: Objects for which we can discard stellar companions down to 3au; RTW2: Objects for which we can discard companions with masses > 13 Mjup as close as 5au; RTW3: Objects for which we can discard stellar companions down to ~10au.