Abstract Cluster environments influence galaxy evolution by curtailing star formation activity, notably through ram-pressure stripping (RPS). This process can leave observable signatures—such as gas tails and truncated gas disks—that are crucial for understanding how RPS affects galaxies. In this study, using spatially resolved spectroscopic data from the SAMI Galaxy Survey, we identify galaxies undergoing or recently affected by RPS in eight nearby clusters (0.029 < z < 0.058), through a visual classification scheme based on the ionised gas (Hα +NIIλ6584) morphologies, split into “unperturbed”, “asymmetric”, and “truncated”. Alongside, we measure non-parametric structural parameters (concentration, asymmetry, and offset between gas and stars) to quantify the ionised gas morphologies. We find that combinations of parameters such as concentration, shape asymmetry, and stellar–ionised gas centre offsets are useful in categorising the degree of RPS in line with their ionised gas morphologies. The projected phase-space analysis shows that asymmetric galaxies are found in a narrow region in cluster-centric distance (0.1 < R/R 200 < 0.6, where R 200 is the characteristic cluster radius) and have a larger dispersion in line-of-sight velocity ( , with σ 200 being the cluster velocity dispersion within R 200 ), compared to the truncated and unperturbed samples that are more broadly distributed and predominantly located at larger cluster-centric distances. This suggests that asymmetric galaxies are likely recent infallers—having crossed within 0.5 R 200 in the past ∼1 Gyr. In terms of star formation activity, we find that the resolved star-forming main sequence (rSFMS; Σ SFR –Σ * ) of unperturbed and RPS candidates (asymmetric and truncated) differ. RPS candidates yield a much steeper rSFMS relation compared to the unperturbed counterparts, primarily emerging from having lower Σ SFR values for the low mass density regime (i.e., log Σ * ≲ 8 M ⊙ kpc –2 ), with the steepest gradient deriving from the truncated sample. Moreover, radial specific star formation rate profiles introduce different trends for unperturbed and RPS candidates. Star formation in RPS candidates is suppressed in the outskirts relative to unperturbed galaxies and is more prominent for the truncated sample compared to the asymmetric counterparts. In contrast, central (i.e., r/r eff < 0.5) star formation activity in RPS candidates is comparable with that in their unperturbed and field counterparts, suggesting no elevated activity. Taken together, this suggests an evolutionary trend linked to the RPS stage, where unperturbed galaxies likely represent recently accreted systems (pre-RPS), while asymmetric and truncated galaxies may correspond to populations undergoing RPS and post-RPS phases, respectively, favouring outside-in quenching.
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