The PSF smoothing effect on concentration-related parameters of high-redshift galaxies in HST and JWST

Aims. We performed a comprehensive investigation of the PSF smoothing effect on the measurement of concentration-related parameters (C, Gini, and M20) of high-redshift galaxies in the HST and JWST surveys. Methods. Our sample contains massive galaxies (10(9.5) M-circle dot <= M-* <= 10(11.5) M-circle dot) from the CANDELS/EGS survey (at redshift 0 < z < 2), and the CEERS survey (at redshift 1 < z < 3). The non-parametric concentration-related parameters (R20, R80, C, Gini, and M20) and the model-dependent parameters (n and Re) of these galaxies were derived from Statmorph and GALFIT, respectively. The best-fit S & eacute;rsic index (n) derived from image modelling is generally robust against the PSF smoothing effect and can be used to describe the intrinsic light distribution of galaxies. On the other hand, the concentration-related parameters are significantly affected by the PSF smoothing effect since they are directly calculated from the pixels of galaxy images. We tried to evaluate the PSF smoothing effect by comparing the concentration-related parameters to the S & eacute;rsic index in both observations and mock images. Results. We find that the concentration index is generally underestimated, especially for smaller galaxies with a higher S & eacute;rsic index (eventually converging to the concentration index of the PSF). However, galaxies with a lower S & eacute;rsic index (n <= 1) or larger relative size (Re/FWHM > 3) are less affected by the PSF smoothing effect. Tests with idealised mock images reveal that overestimating the measured R20/Re ratio leads to underestimating the concentration index C. Another commonly used concentration index C59, derived from R50 and R90 values, is less affected by the PSF. The Gini coefficient and the absolute M20 statistic also show a similar behaviour as the concentration index. Caution should be taken for the possible correction of the concentration-related parameters, where both the relative size and the S & eacute;rsic index of the galaxy are important. We also generated high-redshift artificial images from the low-redshift HST observations and confirm that the traditional correction method that simply adds a single term to the non-parametric indicators of galaxies at higher redshifts is unable to reliably recover the true distribution of the structural parameters. Compared to the HST images, the PSF smoothing is much less severe for images in the CEERS survey (for the short-wavelength filters) due to the much higher spatial resolution. In fact, it is better to use the S & eacute;rsic index rather than the non-parametric morphology indicators to trace the light concentration for galaxies at high redshifts. From the single S & eacute;rsic modelling of the HST and JWST images, we also confirm that galaxies at higher redshifts are more compact with smaller Re. The low-mass galaxies are more disc-like (n similar to 1) compared to the high-mass galaxies that are more spheroid dominated (n similar to 3).