3     -10.2 0.5     -19.4 1.0     -8.9 0.3    103.0   7.0    13
   A     149   53 3      -92 3      -3 3      -9.5 0.7     -20.1 1.1     -7.9 0.3    106.5   7.2    50
   B     317   55 8      -94 4     +10 3      -8.8 1.1     -20.2 1.8     -7.1 0.3    109.5   9.3    98
   C     487   63 11     -97 8     +23 4      -8.2 1.1     -20.9 1.5     -6.1 0.6    118.0   10.0   249
  ---- ----- ---- ---- ----- --- ----- --- ------- ----- ------- ----- ------ ----- ------- ------ -----

\[TabGroups\]

There are no sharp, physically justified boundaries in space between CMG A0, A, B and C and the stars from CMG Z. However, we will show in the following that, on average, they slightly differ not only by their location and kinematics, but also by their average age.

CMG compared with other LCC samples {#comp}
-----------------------------------

Before comparing our results with the work of other authors, we first summarize the selection process that led us to the large moving group CMG. The first selection from [[*Gaia*]{}]{} DR2 was a cone search around $(\alpha,\delta)$ = (186.5, -60.5) with a radius of 20 degrees, trigonometric parallax , and proper motions -43 mas/y $\leq \mu_{\alpha*} \leq$ -20 mas/y ($\mu_{\alpha*} \equiv \mu_\alpha \cos\delta$), and -35 