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Table 2

Cross-match of the Gaia -ESO SB3 and SB4 samples, and Gaia DR3.

Gaia-ESO CNAME Gaia source ID ϖ G GBP GRP RUWE υrad
mas mag mag km s−1
Probable SB3

08202324-1402560(a) 5723402401367964032 0.687 ± 0.036 15.667 1.111 0.954 nan
08393088-0033389(b) 3073616933620127488 0.433 ± 0.032 15.137 0.757 1.078 nan
08402079-0025437 3075120756289226240 0.589 ± 0.041 15.379 0.995 1.068 nan
15120307-4049481 6005054498237096832 2.882 ± 0.633 16.210 1.152 11.683 nan
15420717-4407146(a) 5989143813386060416 0.936 ± 0.085 17.082 1.875 1.006 nan
18170244-4227076 (a) 6724489665257001472 0.514 ± 0.037 15.781 1.098 0.939 nan
21393685-4659598 6563596479474777600 0.575 ± 0.032 15.576 0.990 1.079 nan

Tentative SB3

00195847-5423227 (a) 4923333999386498048 0.945 ± 0.411 15.577 0.919 15.259 nan
15161563-4125518(a) 6004304635606156928 0.388 ± 0.107 16.644 1.280 1.993 nan
16003634-0745523(c) 4349436487865043840 0.051 ± 0.066 16.765 1.097 1.033 nan

Tentative SB4

18263326-3146508 4045322974757410560 0.623 ± 0.669 16.937 1.741 10.934 nan
19243943+0048136(a,b) 4263752096494076160 0.789 ± 0.027 14.792 1.373 0.834 −8.220

Notes. The coluns are the following: Gaia parallax; magnitudes; Renormalised Unit Weight Error (RUWE); and radial velocities. (a)Merle et al. (2017).(b)Merle et al. (2020).(c)Potential binary from proper motion anomaly (Kervella et al. 2019).

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