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Theories that attempt to explain the dynamical relationship between bar andspiral patterns in galactic disks make different predictions about the radialprofile of the pattern speed. These are tested for the H-alpha bar and spiralpatterns of NGC 1365. The radial profile of the pattern speed is measured byfitting mathematical models that are based on the Tremaine-Weinberg method. Theresults show convincing evidence for the bar rotating at a faster rate than thespiral pattern, inconsistent with a global wave mode or a manifold. There isevidence for mode coupling of the bar and spiral patterns at the overlap ofcorotation and inner Lindblad resonances, but the evidence is unreliable andinconsistent. The results are the most consistent with the bar and spiralpatterns being dynamically distinct features. The pattern speed of the barbegins near an ILR and ends near the corotation resonance. The radial profileof the pattern speed beyond the bar most closely resembles what is expected forcoupled spiral modes and tidal interactions.

The Dynamical Relationship Between the Bar and Spiral Patterns of NGC 1365