Abstract
New observations of the distribution of thermal and nonthermal radio-continuum emission in M51 are presented and compared with two optical tracers of spiral structure: the H-alpha emission from giant H II complexes and the dust lanes. The presence of an underlying smooth nonthermal base-disk component of the radio-continuum emission in M51 is confirmed; this component has a morphology similar to the old disk stars in the galaxy. The thermal radio emission in M51 correlates well with the optical H-alpha emission from the giant H II complexes. There is no evidence that similar complexes are present but hidden in the dust. It is confirmed that the ridges in the nonthermal radio emission correspond closely with the dust lanes along major portions of the spiral arms in M51. A number of features not previously recognized are described. Near the dust lane there is evidence that the cool-cloud component appears to separate kinematically from the component in which the nonthermal radio emission is embedded. 24 references.
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