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Understanding how the birthplace of stars affects planet-forming discs isimportant for a comprehensive theory of planet formation. Most stars are bornin dense star-forming regions where the external influence of other stars,particularly the most massive stars, will affect the survival and enrichment oftheir planet-forming discs. Simulations suggest that stellar dynamics play acentral role in regulating how external feedback affects discs, but comparingmodels to observations requires an estimate of the initial stellar density instar-forming regions. Structural analyses constrain the amount of dynamicalevolution a star-forming region has experienced; regions that maintainsubstructure and do not show mass segregation are likely dynamically young, andtherefore close to their birth density. In this paper, we present a structuralanalysis of two clusters in the Carina Nebula, Tr14 and Tr16. We show thatneither cluster shows evidence for mass segregation or a centrally concentratedmorphology, suggesting that both regions are dynamically young. This allows usto compare to simulations from Nicholson et al. (2019) who predict discsurvival rates in star-forming regions of different initial densities. Thesurviving disc fractions in Tr14 and Tr16 are consistent with their predictions(both are $\sim 10$%), supporting a growing body of evidence that thestar-forming environment plays an important role in the survival and enrichmentof protoplanetary discs.

A tale of two clusters: dynamical history determines disc survival in Tr14 and Tr16 in the Carina Nebula