  Stars form in highly-magnetised, supersonic turbulent molecular clouds. Many
of the tools and models that we use to carry out star formation studies rely
upon the assumption of cloud isotropy. However, structures like high-density
filaments in the presence of magnetic fields, and magnetosonic striations
introduce anisotropies into the cloud. In this study we use the two-dimensional
(2D) power spectrum to perform a systematic analysis of the anisotropies in the
column density for a range of Alfv\'en Mach numbers ($\mathcal{M}_A=0.1$--$10$)
and turbulent Mach numbers ($\mathcal{M}=2$--$20$), with 20 high-resolution,
three-dimensional (3D) turbulent magnetohydrodynamic simulations. We find that
for cases with a strong magnetic guide field, corresponding to
$\mathcal{M}_A<1$, and $\mathcal{M}\lesssim 4$, the anisotropy in the column
density is dominated by thin striations aligned with the magnetic field, while
for $\mathcal{M}\gtrsim 4$ the anisotropy is significantly changed by
high-density filaments that form perpendicular to the magnetic guide field.
Indeed, the strength of the magnetic field controls the degree of anisotropy
and whether or not any anisotropy is present, but it is the turbulent motions
controlled by $\mathcal{M}$ that determine which kind of anisotropy dominates
the morphology of a cloud.
