we mention the excellent review of @Preib08 which, in great detail, describes the pre-[[*Gaia*]{}]{} DR2 situation with respect to the Scorpius-Centaurus OB association. From their paper, we have extracted the 121 stars they discuss in LCC and the 90 from UCL. Ninety percent of their stars have masses larger than 0.8 M$_\odot$. Out of the 211 stars, 124 are in our area, 95 fall in the Crux Cone, 90 are in the BS, 82 are young and 62 are members in our CMG.

Among the stars in all these samples which were found in the Crux Cone, the vast majority is also classified as young by us. The confirmation is especially important when we compare with such LCC samples where members were selected by not only using kinematic criteria (i.e., the last six lines in Table \[others\]. Among these stars in the Crux Cone, 96high-mass members found before the advent of [[*Gaia*]{}]{} DR2 form only the tip of the iceberg in the CMG moving group. On the other hand, we have another about 800 stars in our Young sample which are not as strictly co-moving as the stars in CMG. They may have a similar star formation history, but may 