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Physically motivated measurements are crucial for understanding galaxy growthand the role of the environment on their evolution. In particular, the growthof galaxies as measured by their size or radial extent provides an empiricalapproach for addressing this issue. However, the established definitions ofgalaxy size used for nearly a century are ill-suited for these studies becauseof a previously ignored bias. The conventionally-measured radii consistentlymiss the diffuse, outer extensions of stellar emission which harbour keysignatures of galaxy growth, including star formation and gas accretion orremoval. This issue is addressed by examining low surface brightnesstruncations or galaxy "edges" as a physically motivated tracer of size based onstar formation thresholds. Our total sample consists of $\sim900$ galaxies withstellar masses ranging from $10^5 M_{\odot} < M_{\star} < 10^{11} M_{\odot}$.This sample of nearby cluster, group satellite and nearly isolated fieldgalaxies was compiled using multi-band imaging from the Fornax Deep Survey,deep IAC Stripe 82 and Dark Energy Camera Legacy Surveys. Across the full massrange studied, we find that compared to the field, the edges of galaxies in theFornax Cluster are located at 50% smaller radii and the average stellar surfacedensity at the edges are two times higher. These results are consistent withthe rapid removal of loosely bound neutral hydrogen (HI) in hot, crowdedenvironments which truncates galaxies outside-in earlier, preventing theformation of more extended sizes and lower density edges. In fact, we find thatgalaxies with lower HI fractions have edges with higher stellar surfacedensity. Our results highlight the importance of deep imaging surveys to studythe low surface brightness imprints of the large scale structure andenvironment on galaxy evolution.

The edges of galaxies in the Fornax Cluster: Fifty percent smaller and denser compared to the field