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We investigate the structural properties of cluster and group galaxies bystudying the Fornax main cluster and the infalling Fornax A group, exploringthe effects of galaxy preprocessing in this showcase example. Additionally, wecompare the structural complexity of Fornax galaxies to those in the Virgocluster and in the field. Our sample consists of 582 galaxies from the Fornaxmain cluster and Fornax A group. We quantified the light distributions of eachgalaxy based on a combination of aperture photometry, S\'ersic+PSF (pointspread function) and multi-component decompositions, and non-parametricmeasures of morphology (Concentration $C$; Asymmetry $A$, Clumpiness $S$; Gini$G$; second order moment of light $M_{20}$), and structural complexity based onmulti-component decompositions. These quantities were then compared between theFornax main cluster and Fornax A group. The structural complexity of Fornaxgalaxies were also compared to those in Virgo and in the field. Overall, wefind significant differences in the distributions of quantities derived fromS\'ersic profiles ($g'-r'$, $r'-i'$, $R_e$, and $\bar{\mu}_{e,r'}$), andnon-parametric indices ($A$ and $S$) between the Fornax main cluster and FornaxA group. Moreover, we find significant cluster-centric trends with $r'-i'$,$R_e$, and $\bar{\mu}_{e,r'}$, as well as $A$, $S$, $G$, and $M_{20}$ forgalaxies in the Fornax main cluster. We find the structural complexity ofgalaxies increases as a function of the absolute $r'$-band magnitude (andstellar mass), with the largest change occurring between -14 mag $\lesssimM_{r'}\lesssim$ -19 mag. This same trend was observed for galaxies in the Virgocluster and in the field, which suggests that the formation or maintenance ofmorphological structures (e.g. bulges, bar) is largely dependent on the stellarmass of the galaxies, rather than their environment.

The Fornax Deep Survey (FDS) with the VST XI. The search for signs of preprocessing between the Fornax main cluster and Fornax A group