Table 8: The cross-identification of stars considered as candidate members by us, with the radial velocities sudies by Mathieu et al. (1990,1986) and the comparison of those with the parametric ($P_{\rm P}$) and non-parametric ( $P_{\rm NP}$) probabilities. See text for explanation of the agreement index $P_{\rm c}$.
ID $_{\rm BDA}$ ID $_{\rm Zhao}$ $P_{\rm P}$ $P_{\rm NP}$ $P_{\rm c}$ Vr* ID $_{\rm BDA}$ ID $_{\rm Zhao}$ $P_{\rm P}$ $P_{\rm NP}$ $P_{\rm c}$ Vr*
4 818 0.94 0.96 3 34.0 $\pm$2.0 185 958 0.79 0.94 3 33.4 $\pm$0.0
16 829 0.88 0.96 3 33.2 $\pm$0.9 190 989 0.80 0.94 0 43.6 $\pm$0.0 SB
18 521 0.92 0.95 3 32.9 $\pm$0.5 192 603 0.98 0.97 3 32.7 $\pm$1.1
20 834 0.96 0.97 3 33.1 $\pm$1.0 193 999 0.98 0.97 3 33.7 $\pm$0.5
22 839 0.95 0.96 3 34.4 $\pm$1.9 SB1 195 1017 0.97 0.98 3 33.87$\pm$0.12 SB1
28 840 0.97 0.97 3 33.7 $\pm$1.0 210 1005 0.98 0.97 3 33.9 $\pm$1.1
30 845 0.97 0.97 3 33.6 $\pm$0.4 215 608 0.98 0.98 3 33.6 $\pm$0.6
37 846 0.97 0.97 3 33.7 $\pm$0.3 216 1010 0.97 0.98 3 33.03$\pm$0.13 SB1
46 843 0.98 0.97 3 33.8 $\pm$0.1 217 1002 0.97 0.97 3 33.3 $\pm$0.4
48 848 0.96 0.98 3 33.0 $\pm$0.4 218 1006 0.98 0.97 3 34.0 $\pm$0.5
51 849 0.96 0.97 3 34.6 $\pm$0.9 219 1007 0.98 0.98 3 33.4 $\pm$0.3 SB1
54 863 0.95 0.97 3 34.5 $\pm$0.7 223 609 0.68 0.94 3 32.8 $\pm$0.4
55 862 0.75 0.92 0 42.1 $\pm$0.0 SB 224 1011 0.95 0.96 3 32.55$\pm$0.07 SB1
72 876 0.97 0.98 3 33.3 $\pm$0.6 226 1013 0.98 0.98 3 32.5 $\pm$1.0
79 860 0.97 0.98 3 34.1 $\pm$1.7 227 1004 0.98 0.97 3 32.8 $\pm$0.7
84 966 0.78 0.94 3 34.1 $\pm$0.4 231 1029 0.97 0.97 3 32.5 $\pm$0.6
86 933 0.81 0.86 1 27.6 $\pm$0.0 236 1025 0.98 0.98 3 33.82$\pm$0.18 SB1
88 927 0.96 0.97 3 34.13$\pm$0.23 SB2 237 611 0.97 0.98 3 34.7 $\pm$0.7
95 886 0.98 0.98 3 34.7 $\pm$2.4 238 1028 0.75 0.94 3 38.3 $\pm$0.0
96 929 0.96 0.98 3 33.1 $\pm$0.7 241 1027 0.96 0.96 3 33.2 $\pm$0.7
101 930 0.97 0.98 3 32.9 $\pm$0.9 243 1026 0.96 0.96 3 33.4 $\pm$0.5
102 893 0.98 0.97 3 36.17$\pm$0.17 SB1 244 1032 0.93 0.96 3 33.55$\pm$0.05 SB1
104 931 0.95 0.97 3 33.5 $\pm$0.4 248 612 0.98 0.98 3 34.0 $\pm$1.3
105 883 0.80 0.94 3 34.3 $\pm$0.7 252 618 0.97 0.96 3 32.5 $\pm$1.0
108 894 0.51 0.93 2 34.7 $\pm$0.6 255 1043 0.96 0.97 3 31.3 $\pm$0.3
111 891 0.98 0.97 3 33.70$\pm$0.22 SB1 256 226 0.96 0.98 3 33.2 $\pm$0.9
115 918 0.97 0.98 3 34.4 $\pm$0.5 262 1046 0.97 0.97 3 31.6 $\pm$0.7
117 887 0.98 0.98 3 34.4 $\pm$0.3 SB2 266 647 0.78 0.94 3 34.3 $\pm$0.4
119 924 0.97 0.97 3 34.34$\pm$0.21 SB2 271 1058 0.93 0.96 3 34.1 $\pm$0.8
124 912 0.97 0.98 3 29.6 $\pm$0.7 SB 272 645 0.97 0.97 3 31.8 $\pm$0.4
127 911 0.97 0.98 3 33.3 $\pm$0.8 281 1060 0.96 0.97 3 33.4 $\pm$0.8
130 910 0.94 0.98 3 33.7 $\pm$0.7 286 697 0.35 0.92 2 33.6 $\pm$0.5
131 972 0.95 0.96 3 33.3 $\pm$2.0 SB2 287 698 0.98 0.97 3 32.8 $\pm$0.5
134 907 0.98 0.97 3 32.5 $\pm$1.2 SB1 289 683 0.94 0.96 3 32.7 $\pm$0.4
135 908 0.97 0.97 3 34.3 $\pm$0.6 291 700 0.96 0.97 3 34.1 $\pm$0.1
136 974 0.94 0.96 3 32.87$\pm$0.12 SB1 305 133 0.52 0.92 2 34.2 $\pm$0.9
141 947 0.86 0.95 3 33.6 $\pm$0.4 1182 174 0.95 0.98 3 34.6 $\pm$0.9
143 937 0.91 0.96 3 32.93$\pm$0.07 SB1 2079 172 0.98 0.98 3 34.4 $\pm$0.5
149 949 0.98 0.97 3 35.5 $\pm$0.8 2087 211 0.94 0.97 3 31.5 $\pm$3.0
151 971 0.81 0.94 3 33.9 $\pm$0.5 3035 1001 0.98 0.98 3 34.1 $\pm$0.5
157 976 0.98 0.98 3 33.6 $\pm$0.5 3116 642 0.98 0.97 3 33.60$\pm$0.13 SB1
163 995 0.98 0.98 3 33.8 $\pm$0.8 4004 939 0.98 0.98 3 33.48$\pm$0.19 SB2
164 983 0.79 0.94 3 33.3 $\pm$0.4 4096 578 0.97 0.97 3 34.0 $\pm$0.8
166 4 0.97 0.98 3 33.3 $\pm$0.3 7591 135 0.91 0.96 3 33.4 $\pm$0.8
170 953 0.60 0.93 3 33.59$\pm$0.10 SB1 7657 505 0.28 0.87 2 33.2 $\pm$0.9
174 961 0.97 0.98 3 36.2 $\pm$4.5 8402 231 0.83 0.94 3 33.6 $\pm$0.4
176 914 0.97 0.98 3 32.5 $\pm$0.4 SB1 8524 639 0.69 0.89 3 33.6 $\pm$0.7
180 985 0.98 0.97 3 35.0 $\pm$0.8 8571 253 0.94 0.95 3 34.2 $\pm$0.4
181 955 0.98 0.98 3 33.3 $\pm$0.7 8792 282 0.85 0.93 3 33.1 $\pm$0.5
182 956 0.97 0.98 3 32.2 $\pm$2.2 8808 277 0.85 0.94 3 29.6 $\pm$1.0
184 987 0.98 0.97 0 61.4 $\pm$0.0 8832 713 0.97 0.97 3 33.5 $\pm$0.7
(*) Zero errors mean that only one measurement was taken and no dispersion could be calculated. SB1: Single-lined spectroscopic binary. SB2: Double-lined spectroscopic binary.


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