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Lyman-Alpha (Ly$\alpha$) is the strongest emission line in the Universe andis frequently used to detect and study the most distant galaxies. Because Lyais a resonant line, photons typically scatter prior to escaping; thisscattering process complicates the interpretation of Ly$\alpha$ spectra, butalso encodes a wealth of information about the structure and kinematics ofneutral gas in the galaxy. Modeling the Ly$\alpha$ line therefore allows us tostudy tiny-scale features of the gas, even in the most distant galaxies.Curiously, observed Ly$\alpha$ spectra can be modeled successfully with verysimple, homogeneous geometries (such as an expanding, spherical shell), whereasmore realistic, multiphase geometries often fail to reproduce the observedspectra. This seems paradoxical since the gas in galaxies is known to bemultiphase. In this Letter, we show that spectra emerging from extremely clumpygeometries with many clouds along the line of sight converge to the predictionsfrom simplified, homogeneous models. We suggest that this resolves the apparentdiscrepancy, and may provide a way to study the gas structure in galaxies onscales far smaller than can be probed in either cosmological simulations ordirect (i.e., spatially-resolved) observations.

From Mirrors to Windows: Lyman-Alpha Radiative Transfer in a Very Clumpy Medium