  Polycyclic Aromatic Hydrocarbons (PAHs) are ubiquitous complex molecules in
the interstellar medium and are used as an indirect indicator of
star-formation. On the other hand the ultraviolet (UV) emission from the young
massive stars directly traces the star formation activity in a galaxy. The
James Webb Space Telescope (JWST), along with the UltraViolet Imaging Telescope
(UVIT), opened up a new window of opportunity to make a better understanding of
the properties of the PAH molecules associated with the star-forming regions.
In this study, we investigate how the resolved scale properties of PAH
molecules in nearby galaxies are affected by star-formation. We analyze the PAH
features observed at 3.3, 7.7, and 11.3 {\mu}m using F335M, F770W, and F1130W
images obtained from JWST. Additionally, we utilize UVIT images to assess the
star formation associated with these PAH emitting regions. Our study focuses on
three galaxies, namely NGC 628, NGC 1365, and NGC 7496, selected based on the
availability of both JWST and UVIT images. Based on the resolved scale study on
the PAH bright regions using JWST and UVIT images, we found that the fraction
of ionized PAH molecules is high in the star-forming regions with high
{\Sigma}SFR. We observed that emission from smaller PAH molecules is more in
the star-forming regions with higher {\Sigma}SFR. Our study suggests that the
PAH molecules excited by the photons from SF regions with higher {\Sigma}SFR
are dominantly smaller and ionized molecules. UV photons from the star-forming
regions could be the reason for a higher fraction of the ionized PAHs. We
suggest that the effect of high temperature in the star-forming regions and the
formation of smaller PAH molecules in the star-forming regions might also be
resulting in the higher fraction of emission in the F335MPAH band.
