$\leq \mu_{\delta} \leq$ +12 mas/y (see Sec. \[astdet\]). This resulted in the Crux Cone with 20138 objects. Then we applied quality filters as recommended by @2018arXiv180409366L [also described in Sec. \[astdet\]] that led to the Basic sample (BS). These and the other relevant sub-samples are summarized in Table \[downselect\].

  ------------------- -------
  Crux Cone             20138
  Basic sample (BS)      3943
  “Old”                  1284
  “Young”                2659
  CMG                    1844
  ------------------- -------

  : The selection window for the Crux Group of Young Stars (CMG)[]{data-label="downselect"}

The area studied in this paper covers most of LCC and a small part of UCL as shown in Fig. \[SCOCEN\]. In the following we compare the stellar content of our samples with the findings of other authors from the literature. A summary of these comparisons is given in Table \[others\].

  -------------------------- ------ ------ ----- ----- ---- ----- -----
                                                                  
                                                                  
  @1999AJ....117..354D–LCC      180    179   129   123   13   110    72
  @1999AJ....117..354D–UCL      221     19    15    15    1    14    10
  @Hooge00–LCC                 1036   1016   254   247   48   199   120
  @Hooge00–UCL                 1498    174    35    33    4    29    16
  @2011MNRAS.416.3108R          436    156   123   119    8   111    76
  @Mamaj02                      110     50    41    41    2    39    30
  @2012ApJ...746..154P          138     68    50    48    6    42    28
  @2012AJ....144....8S          104     67    57    53    0    53    