DOI: 10.5281/zenodo.14252910
title: Table A.6: Description of the full sample table

description: Notes 

a) ID_star is a unique identifier that sorts the table by right ascension but prioritising that components of the same system (equal ID_system) are together and sorted by decreasing brightness.

b) Name of the star, Simbad-searchable, obeying the following priority (n designates a natural number): Proper name > Variable in constellation (V* V n  Con; but not suspected variables, SV*) > Henry Draper (HD n, with  n <= 225300) > Gliese-Jahreiss (GJ n, only if  n < 4000) > Bonner Durchmusterung (BD±n n) > Luyten (LP n-n) > Giclas (G n-n, only if unique Giclas designation) > Luyten (LHS n) > Other designations in chronological order (Haro, StKM/StM, 1RXS/RXS, HIP, LSPM, PM, NLTT, GSC, TYC, MCC, R78b, I81, 2MUCD) > Catalog identifier (Gaia DR3, 2MASS, UCAC4).

c) Gliese-Jahreiß (GJ) designation entry, when available. This includes the first catalogue by Gliese (1957) and its update (Gliese 1969), the supplement by Wooley et al. (1970), and the succeeding editions (Gliese & Jahreiß 1979).

d) "HHMMm±DDd" are the truncated equatorial coordinates. For close stars with separations less than 5 arcsec, a position of the star in the system is added as "N", "S", "E" or "W".

e) SpTnum = 10.0 for O0.0V, 20.0 for B0.0V, 30.0 for A0.0V, 40.0 for F0.0V, 50.0 for G0.0V, 60.0 for K0.0V, 70.0 for M0.0V, 70.5 for M0.5V, 80.0 for L0. The values 0.0 and 999 are reserved for white dwarfs and stars with a luminosity class other than main sequence (V), respectively. Spectral types were rounded when necessary (e.g. M0.0 instead of M0.1, or M4.0 instead of M3.8). "This work" refers to spectral type photometric estimation from absolute magnitudes as Cifuentes et al. (2020).

f) "Candidate" and "Multiple+" must be read as "new unresolved binary candidate".

g) The system nomenclature follows the scheme in Fig. 11.

h) Definitions of SB1, SB2, ST2, ST3, and SQ are shown in Table A.4.

i) WDS discoverer code or literature reference.

j) Abbreviations follow the scheme outlined in Table 8.

k) id: WDS identifier (see also column Discoverer); comp: Component designations; obs1, obs2: First and last observation years; pa2: Positional angle in the most recent measurement; sep2: Separation in the most recent measurement; mag1, mag2: Magnitudes of the two components. More details can be found in the WDS website.

l) In systems of three or more components, "01" denotes the separation between the closest components, i.e., s01  <  s02.

m) The reference is displayed when the value is not calculated in this work using Gaia data. The reference for s02 is Gaia in all cases. This also applies to the orbital periods.

n) Measured eastward from the north in the epoch 2016.0. In the programmatic computation of this parameter caution must be taken regarding the "quadrant ambiguity", i.e., a 180-deg erroneous difference.

o) For triple or higher-order systems, this association refers to the primary component.

p) Criteria for physical association (crit_association) and statistical metrics from Gaia as described in Table 3 (crit_ruwe, crit_ipd_ruwe, crit_rv, crit_rv_error, crit_ipd_fmp, crit_dupl_source, crit_non_single, crit_DR3_non_single). Orbital: Orbital model for an astrometric binary; OrbitalTargetedSearch: Orbital model for a priori known systems, with a subset containing suffix "Validated"; SB1: Single-lined spectroscopic binary; SB2: Double-lined spectroscopic binary; SB2C: Double-lined spectroscopic binary with circular orbit; AstroSpectroSB1: Combined astrometric and single lined spectroscopic orbital model.

q) It refers to unknown unresolved binaries. That is, if an unresolved companion already exists (e.g. an spectroscopic binary), the value is "false" regardless of the criteria for unresolved binarity (Table 3).

r) Statistics from DR3 related to the criteria for unresolved binarity: astrometric_excess_noise, astrometric_excess_noise_sig, phot_bp_rp_excess_factor, phot_bp_n_blended_transits, phot_rp_n_blended_transits, phot_variable_flag, rv_chisq_pvalue, rv_amplitude_robust, rv_nb_transits, renormalised_gof, astrometric_n_obs_al, astrometric_n_good_obs_al, ipd_gof_harmonic_amplitude, duplicated_source (see Sect. 3.2).

s) G_BP, G, and  G_RP from Gaia DR3 (Gaia Collaboration et al. 2023b); J, H, and Ks from 2MASS (Skrutskie et al. 2006); W1, W2, W3, W4 from AllWISE (Cutri et al. 2014). The photometric uncertainties in the Gaia passbands have been calculated by us ∆lambda = |-2.5 ln(10) ∆F_lambda/F_lambda|, where F_lambda and ∆F_lambda are the flux and its error in the "lambda" passband, using the errors in the corresponding fluxes, and the zero points as provided by VizieR.