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Do spatial distributions of dust grains in galaxies have typical forms, as dospatial distributions of stars? We investigate whether or not the distributionsresemble uniform foreground screens, as commonly assumed by the high-redshiftgalaxy community. We use rest-frame infrared, ultraviolet, and H$\alpha$ lineluminosities of dust-poor and dusty galaxies at z ~ 0 and z ~ 1 to comparemeasured H$\alpha$ escape fractions with those predicted by the Calzettiattenuation formula. The predictions, based on UV escape fractions,overestimate the measured H$\alpha$ escape fractions for all samples. Theinterpretation of this result for dust-poor z ~ 0 galaxies is that regions withionizing stars have more dust than regions with nonionizing UV-emitting stars.Dust distributions for these galaxies are nonuniform. The interpretation of theoverestimates for dusty galaxies at both redshifts is less clear. If theattenuation formula is inapplicable to these galaxies, perhaps thedisagreements are unphysical; perhaps dust distributions in these galaxies areuniform. If the attenuation formula does apply, then dusty galaxies havenonuniform dust distributions; the distributions are more uniform than they arein dust-poor galaxies. A broad range of H$\alpha$ escape fractions at a givenUV escape fraction for z ~ 1 dusty galaxies, if real, indicates diverse dustmorphologies and the implausibility of the screen assumption.

Dusty galaxies and the degeneracy between their dust distributions and the attenuation formula