  The standard paradigm for the formation of the Universe suggests that large
structures are formed from hierarchical clustering by the continuous accretion
of less massive galaxy systems through filaments. In this context, filamentary
structures play an important role in the properties and evolution of galaxies
by connecting high-density regions, such as nodes, and being surrounded by
low-density regions, such as cosmic voids. The availability of the filament and
point critic catalogues extracted by \textsc{DisPerSE} from the
\textsc{Illustris} TNG300-1 hydrodynamic simulation allows a detailed analysis
of these structures. The halo occupation distribution (HOD) is a powerful tool
for linking galaxies and dark matter halos, allowing constrained models of
galaxy formation and evolution. In this work we combine the advantage of halo
occupancy with information from the filament network to analyse the HOD in
filaments and nodes. In our study, we distinguish the inner regions of cosmic
filaments and nodes from their surroundings. The results show that the
filamentary structures have a similar trend to the total galaxy sample covering
a wide range of densities. In the case of the nodes sample, an excess of faint
and blue galaxies is found for the low-mass nodes suggesting that these
structures are not virialised and that galaxies may be continuously falling
through the filaments. Instead, the higher-mass halos could be in a more
advanced stage of evolution showing features of virialised structures.
