  The newest generation of integral field unit spectrographs brings
three-dimensional mapping of nearby galaxies one step closer. While the focus
up to this point was mostly on stars and ionised gas, it is also possible to
look at dust in a new, more complete way. Using MUSE science verification
observations of NGC 5626, we map the interstellar matter in this dusty
lenticular. We use the resolving power of MUSE to measure the optical
attenuation with a spectral resolution of 6.25 \AA, at physical scales of 0.1-1
kpc. The integrated attenuation curve of NGC 5626 shows a smooth, slightly
steeper than Milky Way and SMC attenuation curves. Several sharp features are
superimposed: we measure lower attenuation at spectral emission lines and
higher attenuation for the sodium line doublet. No correlation was observed
between sodium line strength and reddening by dust on spatially resolved
scales. Additionally, the continuum attenuation was found to be independent
from the Balmer decrement (tracing ionised gas attenuation). We model and
interpret the variations in the attenuation curves of each spatial resolution
element of NGC 5626. We find that the amount and distribution of dust along the
line-of-sight is highly degenerate with any variation in the intrinsic
extinction law. Our analysis shows that the interstellar matter in NGC 5626
resides in a regular and well-settled disk. Our results preach caution in the
application of simple recipes to de-redden global galaxy spectra and underlines
the need for more realistic dust geometries when constructing such correction
formulas.
