  To probe the star formation process, we present an observational
investigation of the Pillar IV and an ionized knot HH 216 in the Eagle Nebula
(M16). Pillar IV is known to host a Class I protostar that drives a bipolar
outflow. The outflow has produced the bow shock, HH 216, which is associated
with the red-shifted outflow lobe. The James Webb Space Telescope's near- and
mid-infrared images (resolution $\sim$0.07 arcsec - 0.7 arcsec) reveal the
protostar as a single, isolated object (below 1000 AU). The outer boundary of
Pillar IV is depicted with the 3.3 $\mu$m Polycyclic aromatic hydrocarbon (PAH)
emission. HH 216 is traced with the 4.05 $\mu$m Br$\alpha$ and the radio
continuum emission, however it is undetected with 4.693 $\mu$m H$_{2}$
emission. HH 216 seems to be associated with both thermal and non-thermal radio
emissions. High-resolution images reveal entangled ionized structures (below
3000 AU) of HH 216, which appear to be located toward termination shocks. New
knots in 4.693 $\mu$m H$_{2}$ emission are detected, and are mainly found on
Pillar IV's northern side.
  This particular result supports the previously proposed episodic accretion in
the powering source of HH 216. One part of the ionized jet (extent $\sim$0.16
pc) is discovered on the southern side of the driving source.
  Using the $^{12}$CO($J$ = 1-0), $^{12}$CO($J$ = 3-2), and $^{13}$CO($J$ =
1-0) emission, observational signposts of Cloud-Cloud Collision (or interacting
clouds) toward Pillar IV are investigated. Overall, our results suggest that
the interaction of molecular cloud components around 23 and 26 km s$^{-1}$
might have influenced star formation activity in Pillar IV.
