Canis Major region with Gaia-DR3

We identified two subgroups of CMa stars in our sample labeled as Cluster A and Cluster B. They are located at roughly the same distance (d_A_=1150^+79^_-88_pc and d_B_=1183^+103^_-108_pc) and exhibit similar space motions that can be derived thanks to the precise radial velocities obtained in this study. The subgroups have a mean isochronal age of about 2-3Myr. However, based on infrared photometry we show that Cluster A has a higher fraction of disc-bearing stars suggesting that it could be somewhat younger than Cluster B. Our analysis provides new insights into the stellar population of the Canis Major region, by identifying new members, characterizing their kinematics, and assessing their evolutionary stages.

Future studies incorporating additional data from upcoming Gaia data releases, multi-wavelength and high-resolution spectroscopic observations will be essential for further advancing our understanding of the history of star formation in this region.