Notes. The table provides an identification of the binarity for the seismic stars in the sample. The first four columns provide identifiers for the stars in the form of their Bayer/Flamsteed designation (or primary name according to SIMBAD) and their “HIP”, “WDS”, and “SB9” IDs. Super-scripts of PN or PS on the star’s name refer to their position within (or near when in parenthesis) 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. “P” refers to the binary period, where spectroscopic (“Spec”) periods are obtained from SB9 (unless otherwise stated with a letter reference), with reference to the adopted most recent period determination. Orbital (“Orb”) binary periods are obtained from ORB6 (unless otherwise stated with a letter reference), with non-zero RMSDs between ORB6 and OARMAC entries in parenthesis. “K₁(/K₂)” gives the semi-amplitude(s) corresponding to the P (Spec) reference. “SONG” gives the number of spectra available for the target in the SONG database SODA (https://soda.phys.au.dk/).

^(a)Included in SB9 with reference to Spencer Jones (1928), but more recent spectroscopic analysis is provided by Skuljan et al. (2004);^(b)Adopting the spectroscopic orbital information, Castelaz (1989) provides astrometric binary orbit solution;^(c)ψ¹ Dra is a hierarchical multiple system where the AB system is determined astrometrically (in ORB6), while the AC system is determined spectroscopically by Gullikson et al. (2015);^(d)Adopting the spectroscopic orbital information, Ren & Fu (2013) provides astrometric binary orbit solution;^(e)Found to be SB2 by Katoh et al. (2013), but K₂ is not provided due to weakness of lines;^(f)Fekel et al. (2018) (see also Tokovinin 2013) provides a joint analysis of spectroscopic, astrometric, and visual orbit data;^(g)Adopting the spectroscopic orbital information, Fekel et al. (2007) provides astrometric binary orbit solution;^(h)Tokovinin (2014) provides an orbital period for this SB1 binary (but no semi-amplitude), in agreement with the Gaia DR3 Non-single-star (NNS) period of 524 ± 6 days (Halbwachs et al. 2023);⁽ⁱ⁾Zechmeister et al. (2013);^(j)McLaughlin (1962);^(k)Gontcharov & Kiyaeva (2010);^(l)Adopting the value in OARMAC from Roberts et al. (2011);^(m)Roberts et al. (2016) provides a combined astrometric ans spectroscopic analysis;⁽ⁿ⁾Preliminary period by Schnupp et al. (2010) from 9 yr RV data (no semi-amplitude provided);^(o)Jenkins et al. (2015) provides spectroscopic solution and finds indications of a high eccentricity (ecc~0.84) low-mass companion;^(p)Estimate by Heintz (1974), ORB6 only lists period for BC component of this triple system.

References. (1) Bertiau (1957); (2) Hourihane et al. (2023); (3) Agati et al. (2015); (4) Luck (2017); (5) Pourbaix (2000); (6) Behr et al. (2011); (7) Griffin (1999); (8) Murdoch & Hearnshaw (1993); (9) Ammler-von Eiff & Reiners (2012); (10) Schröder et al. (2009); (11) Griffin (2011); (12) Katoh et al. (2013); (13) Takeda et al. (2005); (14) Halbwachs et al. (2018); (15) Borisov et al. (2023); (16) Duquennoy & Mayor (1991); (17) Batten et al. (1985); (18) Mazeh et al. (2002); (19) Halbwachs et al. (2012); (20) Fekel et al. (2015); (21) Neubauer (1929); (22) Hojjatpanah et al. (2019); (23) Griffin (2001); (24) Bernacca & Perinotto (1970); (25) Díaz et al. (2018); (26) Martínez-Arnáiz et al. (2010); (27) Strassmeier et al. (2023); (28) Jönsson et al. (2020)