  We present a multi-wavelength analysis of the star cluster NGC 2316 and its
surroundings. 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 massive
stars (B2.0V-B1.5V, age ~12 Myr) embedded (AV = 4 mag) within this cluster. The
cluster region still forms young stars even though the most massive star was
born ~12 Myr ago. We also found evidence of positive feedback from these
massive stars. We identified a cold gas/dust lane extending westward from the
cluster. The western end of the dust lane seems to favor low-mass star
formation, whereas the cluster's end favors bit massive star formation, which
seems to have started earlier than the western end. We found an elongated
molecular cloud in this region, characterized by numerous filamentary
structures. The morphology of the filaments, along with position-velocity (pv)
maps, velocity dispersion maps, channel maps, etc., indicate a coalescence of
filaments and a potential longitudinal flow of matter toward the cluster
through the western end of the gas/dust lane. This entire region seems to be a
Hub-filamentary system (HFS), in which the NGC 2316 cluster is probably the hub
and the dark lane is the main filamentary structure. Being the gravity well of
this HFS, star formation started first in the NGC 2316 region and went on to
the other filamentary nodes.
