Notes. ^(a) Asterisks (*) denote M dwarfs unless specified otherwise. Eruptive* denotes eruptive variable stars classified by SIMBAD. ^(b) Distance d (derived from the parallaxes) and Gaia colour G_BP − G_RP of each stellar systems are given by the Gaia Catalogue of Nearby Stars (Gaia Collaboration 2021b), which quotes measurements from Gaia Early Data Release 3 (Gaia Collaboration 2021a). ^(c) Stokes I flux density S_I is given by LoTSS-DR2 (Shimwell et al. 2022). ^(d) X-ray luminosity X_L of each stellar system is given by the Second ROSAT all-sky survey source catalogue (2RXS; Boller et al. 2016), unless specified otherwise. The derivation of the X_L upper limit values for some stellar systems in our sample is described in detail by Callingham et al. (2021b).^† Both M-dwarf components of the binary system GJ 856 have very similar angular separation (≲1″) with the LoTSS radio source. Since the GJ 856 A and GJ 856 B themselves are separated by around 1.25″, we cannot ascertain which is emitting the radio signal (or if both are). Their wide separation (> 10 AU) precludes direct magnetic or chromospheric interactions between them (cf. CAS systems).

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