  Globular clusters (GCs) are found ubiquitously in massive galaxies and due to
their old ages, they are regarded as fossil records of galaxy evolution.
Spectroscopic studies of GC systems are often limited to the outskirts of
galaxies, where GCs stand out against the galaxy background and serve as bright
tracers of galaxy assembly. In this work, we use the capabilities of the Multi
Unit Explorer Spectrograph (MUSE) to extract a spectroscopic sample of 722 GCs
in the inner regions ($\lesssim 3 R_\text{eff}$) of 32 galaxies in the Fornax
cluster. These galaxies were observed as part of the Fornax 3D project, a MUSE
survey that targets early and late-type galaxies within the virial radius of
Fornax. After accounting for the galaxy background in the GC spectra, we
extracted line-of-sight velocities and determined metallicities of a sub-sample
of 238 GCs. We found signatures of rotation within GC systems, and comparing
the GC kinematics and that of the stellar body shows that the GCs trace the
spheroid of the galaxies. While the red GCs prove to closely follow the
metallicity profile of the host galaxy, the blue GCs show a large spread of
metallicities but they are generally more metal-poor than the host.
