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Most stars born in clusters and recent results suggest that star formation(SF) preferentially occurs in subclusters. Studying the morphology and SFhistory of young clusters is crucial to understanding early SF. We identify theembedded clusters of young stellar objects (YSOs) down to M stars, in the HIIregions RCW33, RCW32 and RCW27 of the Vela Molecular Ridge. Our aim is tocharacterise their properties, such as morphology and extent of the clusters inthe three HII regions, derive stellar ages and the connection of the SF historywith the environment. Through public photometric surveys such as Gaia, VPHAS,2MASS and Spitzer/GLIMPSE, we identify YSOs with IR, Halpha and UV excesses, assignature of circumstellar disks and accretion. In addition, we implement amethod to distinguish M dwarfs and giants, by comparing the reddening derivedin several optical/IR color-color diagrams, assuming suitable theoreticalmodels. Since this diagnostic is sensitive to stellar gravity, the procedureallows us to identify pre-main sequence stars. We find a large population ofYSOs showing signatures of circumstellar disks with or without accretion. Inaddition, with the new technique of M-type star selection, we find a richpopulation of young M stars with a spatial distribution strongly correlated tothe more massive population. We find evidence of three young clusters, withdifferent morphology. In addition, we identify field stars falling in the sameregion, by securely classifying them as giants and foreground MS stars. Weidentify the embedded population of YSOs, down to about 0.1 Msun, associatedwith the HII regions RCW33, RCW32 and RCW27 and the clusters Vela T2, Cr197 andVela T1, respectively, showing very different morphologies. Our results suggesta decreasing SF rate in Vela T2 and triggered SF in Cr197 and Vela T1.

astronomy and astrophysics

Low mass star formation and subclustering in the HII regions RCW 32, 33  and 27 of the Vela Molecular Ridge. A photometric diagnostics to identify  M-type stars