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The turbulent dynamics of nearby and extragalactic gas structures can bestudied with the column density power spectrum, which is often described by abroken power-law.In an extragalactic context, the breaks in the power spectrahave been interpreted to constrain the disc scale height, which marks atransition from 2D disc-like to 3D motion. However, this interpretation hasrecently been questioned when accounting for instrumental effects. We usenumerical simulations to study the spatial power spectra of isolated galaxiesand investigate the origins of the break scale. We split the gas into variousphases and analyze the time evolution of the power spectrum characteristics,such as the slope(s) and the break scale. We find that the break scale is phasedependent. The physics traced by the break scale also differ: in the warm gasit marks the transition from 2D (disk-like) to 3D (isotropic) turbulence. Inthe cold gas, the break scale traces the typical size of molecular clouds. Wefurther show that the break scale almost never traces the disc scale height. Westudy turbulent properties of the ISM to show that, in the case where the breakscale traces a transition to isotropic turbulence, the fraction of requiredaccretion energy to sustain turbulent motions in the ISM increasessignificantly. Lastly, we demonstrate through simulated observations that it iscrucial to account for observational effects, such as the beam and instrumentalnoise, in order to accurately recover the break scale in real observations.

The Spatial Power Spectrum and Derived Turbulent Properties of Isolated Galaxies