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We present a detailed analysis of star formation properties of galaxies in anearby ($z\sim0.046$) young ($\sim$0.6 Gyr) post-merger cluster system A3376,with a moderate shock front ( $v_{s}\sim$1630 km/s) observed as symmetric radiorelics. Exploiting the spectroscopic data from the wide-field OmegaWINGS surveyand the associated photometric information, our investigations reveal theplausible effects of the dynamic post-merger environment differing from theputative pre-merger cluster environment. The remnants of the pre-merger relaxedcluster environment are realised through the existence of passive spiralgalaxies located in the central regions of the cluster between the two BCGs. Wediscover A3376 to contain a population of massive $(M_{*}/M_{\odot})>10$) blueregular star-forming spirals in regions of maximum merger shock influence butexhibiting star formation rates similar to those in relaxed clusters at similarepoch. We further discover low-mass (Log $(M_{*}/M_{\odot})\leq 10$) late-typeblue PSBs which could either be formed as a result of rapid quenching oflow-mass spirals following the shock-induced star formation or due to theintense surge in the ICM pressures at the beginning of the merger. With thepossibility of the merger shock affecting high- and low-mass spiralsdifferently, our results bridge the seemingly contradictory results observed inknown merging cluster systems so far and establish that different environmentaleffects are at play right from pre- to post-merger stage.

Passive spirals and shock influenced star formation in the merging cluster A3376