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Using a sample of $>200$ clusters, each with typically $100-200$spectroscopically confirmed cluster members, we search for a signal ofalignment between the Position Angle (PA) of the Brightest Cluster Galaxy (BCG)and the distribution of cluster members on the sky about the cluster centre outto projected distances of 3~R$_{200}$. The deep spectroscopy, combined withcorrections for spectroscopic incompleteness, makes our sample ideal todetermine alignment signal strengths. We also use an SDSS based skeleton of thefilamentary Large Scale Structure (LSS), and measure BCG alignment with thelocation of the LSS skeleton segments on the sky out to projected distances of10~R$_{200}$. The alignment signal is measured using three separate statisticalmeasures; Rao's spacing test (U), Kuiper's V parameter (V), and the Binomialprobability test (P). The significance of the BCG alignment signal with bothcluster members and LSS segments is extremely high (1 in a million chance orless to be drawn randomly from a uniform distribution). We investigate a wideset of parameters that may influence the strength of the alignment signal.Clusters with more elliptical-shaped BCGs show stronger alignment with boththeir cluster members and LSS segments. Also, selecting clusters with closelyconnected filaments, or using a luminosity-weighted LSS skeleton, increases thealignment signal significantly. Alignment strength decreases with increasingprojected distance. Combined, these results provide strong evidence for thegrowth of clusters and their BCGs by preferential feeding along the directionof the filaments in which they are embedded.

BCG alignment with the Locations of Cluster Members and the Large Scale Structure out to 10 R$_{200}$