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We analyse the structure of galaxies with high specific star formation rate(SSFR) in cluster and field environments in the redshift range $0.5<z<1.0$.Recent studies have shown that these galaxies are strongly depleted in denseenvironments due to rapid environmental quenching, giving rise topost-starburst galaxies (PSBs). We use effective radii and S\'ersic indices astracers of galaxy structure, determined using imaging from the UKIDSS UltraDeep Survey (UDS). We find that the high-SSFR galaxies that survive into thecluster environment have, on average, larger effective radii than those in thefield. We suggest that this trend is likely to be driven by the most compactstar-forming galaxies being preferentially quenched in dense environments. Wealso show that the PSBs in clusters have stellar masses and effective radiithat are similar to the missing compact star-forming population, suggestingthat these PSBs are the result of size-dependent quenching. We propose thatboth strong stellar feedback and the stripping of the extended halo acttogether to preferentially and rapidly quench the compact and low-massstar-forming systems in clusters to produce PSBs. We test this scenario usingthe stacked spectra of 124 high-SSFR galaxies, showing that more compactgalaxies are more likely to host outflows. We conclude that a combination ofenvironmental and secular processes is the most likely explanation for theappearance of PSBs in galaxy clusters.

Compact star-forming galaxies preferentially quenched to become PSBs in $z<1$ clusters