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We have measured the radial brightness distributions in the disks of threenearby face-on spirals: M 51, NGC 3631, and NGC 4321 (M 100) in the photometricbands B through I, with the addition of the K band for M 51 only. Themeasurements were made by averaging azimuthally, in three modes, thetwo-dimensional surface brightness over the disks in photometric images of theobjects in each band: (a) over each disk as a whole, (b) over the spiral armsalone, and (c) over the interarm zones alone. From these profiles scale-lengthswere derived for comparison with schematic exponential disk modelsincorporating interstellar dust. These models include both absorption andscattering in their treatment of radiative transfer. The model fits show thatthe arms exhibit greater optical depth in dust than the interarm zones. Theaverage fraction of emitted stellar light in V which is extinguished by dustwithin 3 scale-lengths of the center of each galaxy does not rise above 20% inany of them. We show that this conclusion is also valid for models with similaroverall quantities of dust, but where this is concentrated in lanes. These canalso account for the observed scale-lengths, and their variations.

Scale Lengths in Disk Surface Brightness as Probes of Dust Extinction in Three Spiral Galaxies: M51, NGC 3631, and NGC 4321