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Observations indicate that the central gas discs are smoother in early-typegalaxies than their late-type counterparts, while recent simulations predictthat the dynamical suppression of star formation in spheroid-dominated galaxiesis preceded by the suppression of fragmentation of their interstellar media.The mass surface density power spectrum is a powerful tool to constrain thedegree of structure within a gas reservoir. Specifically here, we focus on thepower spectrum slope and aim to constrain whether the shear induced by adominant spheroidal potential can induce sufficient turbulence to suppressfragmentation, resulting in the smooth central gas discs observed. We computesurface density power spectra for the nuclear gas reservoirs of fourteensimulated isolated galaxies and twelve galaxies observed as part of the mm-WaveInterferometric Survey of Dark Object Masses (WISDOM) project. Both simulatedand observed galaxies range from disc-dominated galaxies to spheroids, withcentral stellar mass surface densities, a measure of bulge dominance, varyingby more than an order of magnitude. For the simulations, the power spectrasteepen with increasing central stellar mass surface density, thereby clearlylinking the suppression of fragmentation to the shear-driven turbulence inducedby the spheroid. The WISDOM observations show a different (but potentiallyconsistent) picture: while there is no correlation between the power spectrumslopes and the central stellar mass surface densities, the slopes scatteraround a value of 2.6. This is similar to the behaviour of the slopes of thesimulated galaxies with high central stellar mass surface densities, and couldindicate that high shear eventually drives incompressible turbulence.

The WISDOM of power spectra: how the galactic gravitational potential impacts a galaxy's central gas reservoir in simulations and observations