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Table 2.

Individual stars mentioned in the text or labelled in figures.

Object A B C D E F G H I
HD 9996 x
HD 47009 x
HD 51684 x
HD 55719 x
HD 59435 x x
HD 61468 x
HD 61513 x
HD 70331 x x
HD 81009 x x
HD 137909 x x x x x
HD 158450 x
HD 168767 x
HD 177268 x
HD 188041 x
HD 200311 x
HD 201601 x
HD 208217 x
HD 318107 x x
2MASS J00283062+6947472 x
2MASS J02594527+5419449 x
2MASS J03001958+4355254 x x
2MASS J03080905+4355586 x
2MASS J03112102+6310394 x
2MASS J03414761+2335305 x
2MASS J04140370+4941107 x
2MASS J05482124+0305160 x
2MASS J06055681+1917131 x
2MASS J06352208+3351329 x
2MASS J07175283+1347078 x
2MASS J07390490+4711571 x
2MASS J16241403–4044107 x x x
2MASS J17355458–3350564 x
2MASS J17594524+0302056 x
2MASS J18061507+0237308 x
2MASS J18151324+0121014 x x
2MASS J18171434+0013052 x x
2MASS J18261274–0646548 x x x
2MASS J20191831+2354023 x x
2MASS J21090244+4844449 x
2MASS J21460991+5247363 x
2MASS J22480641+5906428 x

Notes. A: not in Gaia DR2 (Sects. 2 and 2.4, Figs. 3 and 4), B: no Gaia DR2 parallax and largest RUWE (Sect. 2.1, Figs. 3 and 4), C: negative Gaia DR2 parallax (Sects. 2.1 and 2.4, Figs. 3, 5, 7, and 18), D: brightest star, RUWE extrapolated (Sects. 2.1, 2.4, and 3, Figs. 5 and 8), E: low number of visibility_periods_used (Sect. 2.1, Fig. 5), F: known or suspected binary (Sects. 2.2, 2.4, and 4.1, Figs. 5 and 7), G: open cluster member (Sect. 2.3, Table 3), H: CMD/HRD outlier (Sect. 4.1, Figs. 12 and 15), I: outlier in Teff − BP − RP or MG − Lum relation (Sect. 4.1, Figs. 16 and 17).

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