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Table 2.

Solutions from the combination of Gaia NSS astrometric solutions with APOGEE double-lined spectroscopy.

Gaia DR3 ID q σq 1 σ1 2 σ2 β σβ F2
839401128363085568 (a) 0.9143 0.0993 0.6225 0.1162 0.5692 0.0918 0.3865 0.0266 4.03
683525873153063680 0.9376 0.0496 0.5124 0.1037 0.4804 0.0951 0.3985 0.0167 1.72
702393458327135360 0.9398 0.0252 1.4875 0.5001 1.3980 0.4663 0.3871 0.0186 4.53
790545256897189760 0.8549 0.0846 0.4236 0.0870 0.3621 0.0618 0.2850 0.0263 1.20
794359875050204544 0.8824 0.1294 1.1746 0.3294 1.0365 0.2566 0.2676 0.0360 0.99
824315485231630592 0.9035 0.3744 0.9467 0.2152 0.8554 0.2087 0.3104 0.1036 3.92
901170214141646592 0.8396 0.1134 0.9309 0.2506 0.7815 0.1951 0.2330 0.0404 0.46
1267970076306377344 0.6633 0.0586 1.1378 0.2014 0.7547 0.0912 0.0703 0.0157 0.61
1636132061580415488 0.7176 0.1342 1.1046 0.4127 0.7927 0.2574 0.1488 0.0446 3.24
2134829544776833280 0.7721 0.0680 0.8751 0.1245 0.6757 0.0738 0.1505 0.0251 0.73
2705239237909520128 0.5293 0.1035 0.2336 0.0683 0.1236 0.0326 0.1993 0.0427 0.53
3847995791877023104 0.8387 0.0788 1.1446 0.2029 0.9600 0.1550 0.3167 0.0244 1.05
5285071954833306368 (b) 0.7905 0.1019 0.4609 0.1058 0.3643 0.0853 0.1499 0.0416 1.58

Notes.

(a)

q is the mass ratio, ℳ1 is the mass of the primary, ℳ2 is the mass of the secondary (in ℳ), and β is the flux fraction of the secondary. σq, σ1, σ2, and σβ are their associated uncertainties. F2 is the goodness-of-fit estimator. Particular case for which the eccentricity was fixed to 0.

(b)

Mass-luminosity outlier, removed from the study in Sect. 5. The full table including the correlations and the orbital parameters is available at the CDS.

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