[10] The Pavo–Indus Supercluster exhibits a wall[11][12] or filamentary[13][14][15] structure that extends to a total length of 66 Mpc (215 Mly).

[13] In 1983, in a paper by Winkler et al it was suggested based on redshift maps of the distribution of galaxies that the Pavo–Indus Supercluster may be connected to the Centaurus Supercluster.

[18][17] This wall encompasses the Pavo–Indus supercluster through the Norma Cluster, passing the ZOA in the Great Attractor region, to meet up with the Centaurus–Crux Cluster at a redshift at about 5,700–6,200 km/s s and the CIZA J1324.7−5736 cluster at a redshift of 5700 km/s[17] while also splitting off to form the Centaurus Wall[19] passing the galactic plane to meet up with Centaurus Cluster[20] where the supercluster originates.

[13] Di Nel la H. et al found no evidence of a connection between Pavo–Indus and the Perseus–Pisces Supercluster.

[11] However, Tully et al. revealed the existence of a filamentary extension of the Pavo–Indus Supercluster known as the Arch[10] that caps the Local Void in the supergalactic north and provides a connection to the Perseus–Pisces Supercluster[14][15] before terminating close to the NGC 7242 Cluster.