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Galaxies that abruptly interrupt their star formation in < 1.5 Gyr presentrecognizable features in their spectra (no emission and Hd in absorption) andare called post starburst (PSB) galaxies. By studying their stellar populationproperties and their location within the clusters, we obtain valuable insightson the physical processes responsible for star formation quenching. We presentthe first complete characterization of PSB galaxies in clusters at 0.04 < z <0.07, based on WINGS and OmegaWINGS data, and contrast their properties tothose of passive (PAS) and emission line (EML) galaxies. For V < 20, PSBsrepresent 7.2 +/- 0.2% of cluster galaxies within 1.2 virial radii. Theirincidence slightly increases from the outskirts toward the cluster center andfrom the least toward the most luminous and massive clusters, defined in termsof X-ray luminosity and velocity dispersion. The phase-space analysis andvelocity dispersion profile suggest that PSBs represent a combination ofgalaxies with different accretion histories. Moreover, PSBs with the strongestHd are consistent with being recently accreted. PSBs have stellar masses,magnitudes, colors and morphologies intermediate between PAS and EML galaxies,typical of a population in transition from being star forming to passive.Comparing the fraction of PSBs to the fraction of galaxies in transition onlonger timescales, we estimate that the short timescale star-formationquenching channel contributes two times more than the long timescale one to thegrowth of the passive population. Processes like ram-pressure stripping andgalaxy-galaxy interactions are more efficient than strangulation in affectingstar formation.

OmegaWINGS: The first complete census of post starburst galaxies in clusters in the local universe