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Spectra of the highest redshift galaxies taken with JWST are now allowing usto see into the heart of the reionization epoch. Many of these observedgalaxies exhibit strong damping wing absorption redward of their Lyman-$\alpha$emission. These observations have been used to measure the redshift evolutionof the neutral fraction of the intergalactic medium and sizes of ionizedbubbles. However, these estimates have been made using a simple analytic modelfor the intergalactic damping wing. We explore the recent observations withmodels of inhomogeneous reionization from the Sherwood-Relics simulation suite.We carry out a comparison between the damping wings calculated from thesimulations and from the analytic model. We find that although the agreement isgood on the red side of the Lyman-$\alpha$ emission, there is a discrepancy onthe blue side due to residual neutral hydrogen present in the simulations,which saturates the intergalactic absorption. For this reason, we find that itis difficult to reproduce the claimed observations of large bubble sizes at z ~7, which are driven by a detection of transmitted flux blueward of theLyman-$\alpha$ emission. We suggest instead that the observations can beexplained by a model with smaller ionized bubbles and larger intrinsicLyman-$\alpha$ emission from the host galaxy.

JWST observations of galaxy damping wings during reionization interpreted with cosmological simulations