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A 850 micron map of the interacting spiral galaxy M51 shows well-definedspiral arms, closely resembling the structures seen in CO and HI emission.However, most of the 850 micron emission originates in an underlyingexponential disk, a component that has not been observed before in a face-ongalaxy at these wavelengths. The scale-length of this disk is 5.45 kpc, whichis somewhat larger than the scale-length of the stellar disk, but somewhatsmaller than that of atomic hydrogen. Its profile can not be explained solelyby a radial disk temperature gradient but requires the underlying dust to havean exponential distribution as well. This reinforces the view that the submmemission from spiral galaxy disks traces total hydrogen column density, i.e.thesum of H2 and HI. A canonical gas-to-dust ratio of 100+/-26 is obtained forkappa(850)=1.2 g**-1 cm**2, where kappa(850) is the dust opacity at 850 micron.Comment: accepted by A&A, 8 page

A submillimeter exponential disk in M 51: Evidence for an extended cold dust disk