  In galactic disks, galactic rotation sets the bulk motion of gas, and its
energy and momentum can be transferred toward small scales. Additionally, in
the interstellar medium, random and noncircular motions arise from stellar
feedback, cloud-cloud interactions, and instabilities, among other processes.
Our aim is to comprehend to which extent small-scale gas dynamics is decoupled
from galactic rotation. We study the relative contributions of galactic
rotation and local noncircular motions to the circulation of gas, $\Gamma$, a
macroscopic measure of local rotation, defined as the line integral of the
velocity field around a closed path. We measure the circulation distribution as
a function of spatial scale in a set of simulated disk galaxies and we model
the velocity field as the sum of galactic rotation and a Gaussian random field.
The random field is parameterized by a broken power law in Fourier space, with
a break at the scale $\lambda_c$. We define the spatial scale $\lambda_{\rm
eq}$ at which galactic rotation and non-circular motions contribute equally to
$\Gamma$. For our simulated galaxies, the gas dynamics at the scale of
molecular clouds is usually dominated by noncircular motions, but in the center
of galactic disks galactic rotation is still relevant. Our model shows that the
transfer of rotation from large scales breaks at the scale $\lambda_c$ and this
transition is necessary to reproduce the circulation distribution. We find that
$\lambda_{\rm eq}$, and therefore the structure of the gas velocity field, is
set by the local conditions of gravitational stability and stellar feedback.
