  Stellar population synthesis (SPS) is essential for understanding galaxy
formation and evolution. However, the recent discovery of rotation-driven
phenomena in star clusters warrants a review of uncertainties in SPS models
caused by overlooked factors, including stellar rotation. In this study, we
investigate the impact of rotation on SPS specifically using the PARSEC V2.0
rotation model and its implications for high redshift galaxies with the JWST.
Rotation enhances the ultraviolet (UV) flux for up to $\sim 400$ Myr after the
starburst, with the slope of UV increasing as the population gets faster
rotating and more metal-poor. Using the Prospector tool, we construct simulated
galaxies and deduce their properties associated with dust and star formation.
Our results suggest that rapid rotation models result in a gradual UV slope up
to 0.1 dex higher and an approximately 50\% increase in dust attenuation for
identical wide-band spectral energy distributions. Furthermore, we investigate
biases if the stellar population should be characterized by rapid rotation and
demonstrate that accurate estimation can be achieved for rotation rates up to
$\omega_\text{i}=0.6$. Accounting for the bias in the case of rapid rotation
aligns specific star formation rates more closely with predictions from
theoretical models. Notably, this also implies a slightly higher level of dust
attenuation than previously anticipated, while still allowing for a `dust-free'
interpretation of the galaxy. The impact of rapid rotation SPS models on the
rest-UV luminosity function is found to be minimal. Overall, our findings have
potentially important implications for comprehending dust attenuation and mass
assembly history in the high-redshift Universe.
