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Observations of high-redshift galaxies with unprecedented detail have nowbeen rendered possible with JWST. However, accurately quantifying theirmorphology remains uncertain due to potential biases and uncertainties. Toaddress this issue, we used a sample of 1816 nearby DESI galaxies, with a massrange of $10^{9.75-11.25}M_{\odot}$, to compute artificial images of galaxiesof the same mass located at $0.75\leq z\leq 3$ and observed at rest-frameoptical wavelength in CEERS. We analyzed the effects of cosmological redshifton the measurements of Petrosian radius ($R_p$), half-light radius ($R_{50}$),asymmetry ($A$), concentration ($C$), axis ratio ($q$), and S\'ersic index($n$). Our results show that $R_p$ and $R_{50}$, calculated usingnon-parametric methods, are slightly overestimated due to PSF smoothing, while$R_{50}$, $q$, and $n$ obtained through model fitting does not exhibitsignificant biases. We improve the computation of $A$ by incorporating a moreaccurate noise effect removal procedure. Due to PSF asymmetry, there is a minoroverestimation of $A$ for intrinsically symmetric galaxies. However, forintrinsically asymmetric galaxies, PSF smoothing dominates and results in anunderestimation of $A$, an effect that becomes more significant with higherintrinsic $A$ or at lower resolutions. Moreover, PSF smoothing also leads to anunderestimation of $C$, which is notably more pronounced in galaxies withhigher intrinsic $C$ or at lower resolutions. We developed functions based onresolution level, defined as $R_p/$FWHM, for correcting these biases and theassociated statistical uncertainties. Applying these corrections, we measuredthe bias-corrected morphology for the simulated CEERS images and we find thatthe derived quantities are in good agreement with their intrinsic values --except for $A$, which is robust only for angularly large galaxies where$R_p/{\rm FWHM}\geq 5$.

Redshifting galaxies from DESI to JWST CEERS: Correction of biases and uncertainties in quantifying morphology