  Nuclear star clusters (NSCs) are found in at least 70% of all galaxies, but
their formation path is still unclear. In the most common scenarios, NSCs form
in-situ from the galaxy's central gas reservoir, through merging of globular
clusters (GCs), or through a combination of the two. As the scenarios pose
different expectations for angular momentum and stellar population properties
of the NSC in comparison to the host galaxy and the GC system, it is necessary
to characterise the stellar light, NSC, and GCs simultaneously. Wide-field
observations with modern integral field units such as the Multi Unit
Spectroscopic Explorer (MUSE) allow to perform such studies. However, at large
distances, NSCs usually are not resolved in MUSE observations. The particularly
large NSC (R_eff $\sim$ 66 pc) of the early-type galaxy FCC47 at distance of
$\sim$ 20 Mpc is an exception and is therefore an ideal laboratory to constrain
NSC formation of external galaxies.
