Radial distributions of arm–gas offsets as an observational test of spiral theories

Abstract

Abstract Theories of stellar spiral arms in disk galaxies can be grouped into two classes based on the longevity of a spiral arm. Although the quasi-stationary density wave theory supposes that spirals are rigidly rotating, long-lived patterns, the dynamic spiral theory predicts that spirals are differentially rotating, transient, recurrent patterns. In order to distinguish between the two spiral models from observations, we performed hydrodynamic simulations with steady and dynamic spiral models. Hydrodynamic simulations in steady spiral models demonstrated that the dust lane locations relative to the stellar spiral arms (hereafter, arm–gas offsets) depend on radius, regardless of the strength and pitch angle of the spiral and the model of the interstellar medium. In contrast, we found that the dynamic spiral models show no systematic radial dependence of the arm–gas offsets. The arm–gas offset radial profile method, together with the other test methods, will help us to distinguish between the two spiral models in observed spiral galaxies.