Notes. The table provides an identification of the exoplanets and their hosts for the seismic stars in the sample. The stars are ordered according to their V-band brightness. The first two columns provide identifiers for the stars in the form of their Bayer/Flamsteed designation (or primary name according to SIMBAD) and their ‘“HIP” IDs. Super-scripts of PN or PS on the star’s name refer to their position within (or near when in parentheses) the northern (N) or southern (S) PLATO fields (see Table D.2). “V” gives the V-band magnitude, “ν_max” (central value only) is adopted from Table D.1. “Known Seismic” denotes with an X (otherwise an O) if the star is a know asteroseismic target (see Table D.1); “Binary” denotes with an X (otherwise an O) if the star is identified as being part of a binary or multiple star system, and here an asterics (*) indicates that orbital information is available in Table D.5; “HWO” indicates if the star is part of the Mamajek & Stapelfeldt (2024) HWO target list, and if so provides its tier; “Planets” gives the number of identified exoplanets; “Reference” provides the reference(s) for the identified exoplanet(s). ^(†)see Appendix E; ^(a)A faint M4 dwarf companion star (GJ 442 B) at a distance of ~212 AU (Raghavan et al. 2010); ^(b)Loutrel et al. (2011) identified a brown dwarf companion (HD 46588 B; spT L9), one of the few known brown dwarfs at the L/T transition for which both age and distance estimates are available; ^(c)A low-mass K-M dwarf companion star (LHS 1021 / HD 142 B) (Eggenberger et al. 2007; Mugrauer 2019); ^(d)A faint M4.5V dwarf companion star (G 125-55 / GJ 777 B) at a distance of ~2849 AU, which in turn could be an unresolved binary with a similar companion (Mason et al. 2014); ^(e)A potential third planet was identified by Hirsch et al. (2021); ^(f)A wide-separation (a~2460 AU) L-type companion (Wilson et al. 2001; Mugrauer et al. 2004), and another (a~219 AU) proposed candidate companion (Roberts et al. 2011; Fontanive et al. 2019); ^(g)Wittenmyer et al. (2019) finds indications of another Jupiter-mass exoplanet (HD 89744 c) at a separation of 8.3 ± 1.8 AU and with an orbital period of 6974 ± 2161 days; ^(h)A co-moving mid-M-dwarf companion (HD 16417 B) detected by Mugrauer et al. (2004); ⁽ⁱ⁾A wide-separation (a~21,756 AU) companion candidate (likely a mid-M-dwarf) was identified by Venner et al. (2021) (see also El-Badry et al. 2021); ^(j)A wide-separation (a~11,000 AU) M2.5V companion (Raghavan et al. 2006; Montes et al. 2018); ^(k)Benedict et al. (2010) finds indications in the RV residuals of a possible third planetary companion at a period of ~194 days and an inferred a~0.75 AU.

References. (1) Butler et al. (1997); (2) Butler et al. (1999); (3) Pepe et al. (2011); (4) Feng et al. (2017); (5) Nari et al. (2025); (6) Rosenthal et al. (2021); (7) Desort et al. (2008); (8) Vogt et al. (2010); (9) Tinney et al. (2011); (10) Marcy & Butler (1996); (11) Butler & Marcy (1996); (12) Fischer et al. (2002); (13) Gregory & Fischer (2010); (14) Mayor et al. (2004); (15) Galland et al. (2005); (16) Butler et al. (2001); (17) McCarthy et al. (2004); (18) Santos et al. (2004); (19) Pepe et al. (2007); (20) Noyes et al. (1997); (21) Fulton et al. (2016); (22) Brewer et al. (2023); (23) Šubjak et al. (2023); (24) Mayor & Queloz (1995); (25) Udry et al. (2019); (26) Gandolfi et al. (2018); (27) Jones et al. (2002); (28) Hatzes et al. (2022); (29) Feng et al. (2022); (30) Tinney et al. (2002); (31) Wittenmyer et al. (2012); (32) Barnes et al. (2023); (33) Naef et al. (2003); (34) Vogt et al. (2005); (35) Korzennik et al. (2000); (36) Fischer et al. (2009); (37) O’Toole et al. (2009); (38) Kane et al. (2019); (39) Fischer et al. (2001); (40) Fischer et al. (2003).