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) Total flux density S_I is given by the VLASS Quick Look (QL) catalogue (Gordon et al. 2021). S_I from Epoch 1 is adjusted to S_{VLASS Ep.1} = 0.87S_I, as the Epoch 1 flux densities in the VLASS Quick Look imaging are known to be systematically underestimated due to multiple calibration issues (e.g. an antenna pointing error that affected two-thirds of the antennas), which were fixed for subsequent campaigns of VLASS (see Lacy et al. 2019 and Gordon et al. 2021 for more details). The Stokes I flux density from Epoch 2 is unaffected by these issues (i.e. S_{VLASS Ep.2} = S_I). ^(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 upper limits of X_L for LP 732-30 and 2MASS J13582164-0046262 are derived assuming the 2RXS flux limit ≈10⁻¹³ erg cm⁻² s⁻¹ (Boller et al. 2016). ^(e) In the case where a stellar radio source is detected in both Epochs 1 and 2, we choose the epoch that contains a greater value of S_I.^† For the TWA 5 system, there exists a very young brown dwarf companion TWA 5 B of the primary T Tauri star TWA 5 A, with an angular separation of around 2″. Their very large separation (> 100 AU) precludes any magnetic or chromospheric interactions between them. Therefore, the dominant radio emission must be isolated to either component. Due to their proximity and the fact that these two types of YSOs are both capable of generating strong radio emission, it is possible that TWA 5 B may contribute to the radio emission as well. However, since the VLASS radio source is located much closer to A than to B (see Appendix B.4 for more details), we conclude the TTS is indeed the predominant radio emitter.

References. (1) Samus’ et al. (2017); (2) Reid et al. (1995); (3) Newton et al. (2014); (4) Newton et al. (2014); (5) Deshpande et al. (2012); (6) Davison et al. (2015); (7) Davison et al. (2015); (8) Özeren et al. (1999); (9) Davison et al. (2015); (10) Baron et al. (2019); (11) Baron et al. (2019); (12) Newton et al. (2014); (13) Gray et al. (2006); (14) Scholz et al. (2005); (15) Lepine et al. (2013); (16) Fuhrmann et al. (2016); (17) Shkolnik et al. (2009); (18) Alfonso-Garzón et al. (2012); (19) Alonso-Floriano et al. (2015); (20) Clark et al. (2022); (21) Bowler et al. (2019); (22) Naftilan & Fairchild (1993); (23) Gigoyan et al. (2010); (24) Shkolnik et al. (2009); (25) Petit et al. (2014); (26) Shkolnik et al. (2009); (27) Alekseev & Kozlova (2000); (28) Strassmeier & Rice (2003); (29) Gray et al. (2003); (30) Shkolnik et al. (2009); (31) Newton et al. (2014); (32) Kozhevnikova & Alekseev (2015); (33) Garcia-Alvarez et al. (2003); (34) Bychkov et al. (2021); (35) Torres et al. (2006); (36) Fekel et al. (2005a); (37) Tokovinin (2018); (38) Bowler et al. (2019); (39) Shkolnik et al. (2017); (40) Cutispoto (1995); (41) Shkolnik et al. (2009); (42) Reid et al. (2007); (43) Cutispoto et al. (1999); (44) Alonso-Floriano et al. (2015); (45) Lepine et al. (2013); (46) Makarov (2003); (47) Berdyugina et al. (1998); (48) Pourbaix et al. (2004); (49) Alonso-Floriano et al. (2015); (50) Riaz et al. (2006); (51) Favata et al. (1997); (52) Zboril et al. (2005); (53) Strassmeier et al. (2012); (54) Reid & Gizis (2005); (55) Pribulla et al. (2009); (56) Fekel (1996); (57) Gagné et al. (2015); (58) Riedel et al. (2017); (59) Avvakumova et al. (2013); (60) Eker & Doherty (1987); (61) Patel et al. (2016); (62) Alonso-Floriano et al. (2015); (63) Wang et al. (2022); (64) Riaz et al. (2006); (65) Neuhäuser et al. (2000); (66) Freund et al. (2022); (67) Callingham et al. (2021b); (68) Schmitt et al. (1995); (69) Schmitt et al. (1995); (70) Berger et al. (2008); (71) Webb et al. (2020); (72) Callingham et al. (2021b);