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We present a multi-wavelength analysis of the star cluster NGC 2316 and itssurroundings. We estimated the physical parameters of the NGC 2316 cluster,including its shape (elongated), size (Rcluster = 0.4 pc), distance (1.3 +/-0.3 kpc), and minimum reddening (AV = 1.55 mag). We discovered two massivestars (B2.0V-B1.5V, age ~12 Myr) embedded (AV = 4 mag) within this cluster. Thecluster region still forms young stars even though the most massive star wasborn ~12 Myr ago. We also found evidence of positive feedback from thesemassive stars. We identified a cold gas/dust lane extending westward from thecluster. The western end of the dust lane seems to favor low-mass starformation, whereas the cluster's end favors bit massive star formation, whichseems to have started earlier than the western end. We found an elongatedmolecular cloud in this region, characterized by numerous filamentarystructures. The morphology of the filaments, along with position-velocity (pv)maps, velocity dispersion maps, channel maps, etc., indicate a coalescence offilaments and a potential longitudinal flow of matter toward the clusterthrough the western end of the gas/dust lane. This entire region seems to be aHub-filamentary system (HFS), in which the NGC 2316 cluster is probably the huband the dark lane is the main filamentary structure. Being the gravity well ofthis HFS, star formation started first in the NGC 2316 region and went on tothe other filamentary nodes.

Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316