  We analyse the joint distribution of dust attenuation and projected axis
ratios, together with galaxy size and surface brightness profile information,
to infer lessons on the dust content and star/dust geometry within star-forming
galaxies at 0 < z <2.5. To do so, we make use of large observational datasets
from KiDS+VIKING+HSC-SSP and extend the analysis out to redshift z = 2.5 using
the HST surveys CANDELS and 3D-DASH. We construct suites of SKIRT radiative
transfer models for idealized galaxies observed under random viewing angles
with the aim of reproducing the aforementioned distributions, including the
level and inclination dependence of dust attenuation. We find that
attenuation-based dust mass estimates are at odds with constraints from
far-infrared observations, especially at higher redshifts, when assuming smooth
star and dust geometries of equal extent. We demonstrate that UV-to-near-IR and
far-infrared constraints can be reconciled by invoking clumpier dust geometries
for galaxies at higher redshifts and/or very compact dust cores. We discuss
implications for the significant wavelength- and redshift-dependent differences
between half-light and half-mass radii that result from spatially varying dust
columns within -- especially massive -- star-forming galaxies.
