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Minor mergers have been proposed as the driving mechanism for the size growthof quiescent galaxies with decreasing redshift. The process whereby largestar-forming galaxies quench and join the quiescent population at the largesize end has also been suggested as an explanation for this size growth. Giventhe clear association of quenching with clusters, we explore this mechanism bystudying the structural properties of 23 spectroscopically identified recentlyquenched (or "poststarburst" (PSB)) cluster galaxies at $z\sim1$. Despite clearPSB spectral signatures implying rapid and violent quenching, 87\% of thesegalaxies have symmetric, undisturbed morphologies in the stellar continuum.Remarkably, they follow a mass-size relation lying midway between thestar-forming and quiescent field relations, with sizes $0.1$ dex smaller than$z\sim1$ star-forming galaxies at log$(M_{*}/M_{\odot})=10.5$. This implies arapid change in the light profile without directly effecting the stellardistribution, suggesting changes in the mass-to-light ratio gradients acrossthe galaxy are responsible. We develop fading toy models to explore howstar-forming galaxies move across the mass-size plane as their stellarpopulations fade to match those of the PSBs. "Outside-in" fading has thepotential to reproduce the contraction in size and increase in bulge-dominanceobserved between star-forming and PSB cluster galaxies. Since cluster PSBs lieon the large size end of the quiescent mass-size relation, and our previouswork shows cluster galaxies are smaller than field galaxies, the sizes ofquiescent galaxies must grow both from the quenching of star-forming galaxiesand dry minor mergers.

HST/WFC3 grism observations of $z\sim1$ clusters: evidence for evolution in the mass-size relation of quiescent galaxies from poststarburst galaxies