Galaxy clusters form in dense regions of dark matter halos. These halos presumably grow by accreting smaller halos, which are preferentially accreted along the direction of cosmic filaments. In this scenario, halos are not expected to be spherical. Theoretical studies have shown that the major axis of cluster central galaxies tends to align with the major axis of halos. Likewise, the distribution of red cluster satellites tends to be elongated in the direction of the halo elongation. Several observational studies support the theoretical results, with alignment detected between cluster central and satellite galaxy distributions. Utilising J-PLUS and an associated cluster catalogue currently in development, we intend to further study the link between halos and galaxies. In this poster we present preliminary results using another cluster catalogue for cluster selection.