Age spread and sequential star formation in the young cluster NGC 2264

We investigate the structure and star formation history of the NGC 2264 cluster (3 Myr). We combine spectroscopic T_eff with multi-color photometry to derive homogeneous extinction and stellar parameters for 655 cluster members (M_star = 0.2-1.8 M_☉). We infer an intrinsic age spread of ∼4 Myr across the cluster. NGC 2264 members were born in the course of sequential star formation activity, which still continues in the most embedded regions of the cluster. We find evidence for photoevaporation effects driven by OB stars in the region that locally impact the timescales for disk evolution within the cluster