2025MNRAS.540.3661L

During the fall of late-type galaxies into clusters, they can experiment a variety of evolutionary mechanisms according to their local environment. Consequently, studying the ultraviolet (UV) emission and the cold gas of late-type galaxies provide key insights in the evolution of short-lived starburst and galaxy quenching. In this work, we conducted a study of two 28 arcmin fields observed with Ultra Violet Imaging Telescope-AstroSat in the central region of the Abell cluster A496 ($z=0.033$), including H I data from National Radio Astronomy Observatory (NRAO) Very Large Array (VLA). We reported 22 cluster members detected in far-ultraviolet (FUV); all of them are detected in H I, or have upper limits for the H I-mass. We find our FUV detected galaxies generally have higher specific star formation rates (sSFRs) than other star-forming galaxies. Most of the FUV galaxies with masses above 10$^9$$\mathrm{M}_{\odot }$ and showing high sSFR have no close neighbours, pointing at RPS as the dominant mechanism affecting them. In contrast, most of the low-mass FUV objects present at least one companion, suggesting that tidal interactions also play an important role in the triggering of infalling galaxies. Combining the FUV-SFR with the H I properties of the observed galaxies in A496, we identify an evolutionary sequence consisting of five stages: (1) Pre-triggering, (2) Initial SF-triggering, (3) Peak of star-formation, (4) SF-fading, and (5) SF-quenching. During this path, normal gas-rich objects reach a gas-deficiency phase with SFR well below the main sequence. This process, prior to becoming a full passive galaxy, can be accomplished within a few 10$^{8}$ yr.