survey are conceived to reach the necessary accuracy of all of the above quantities, as will be outlined in the next Sections.

Finally, we will not only measure statistically the environmental effects on galaxy properties on such large scales, but also to ‘catch in the act’ the direct interaction of supercluster galaxies with their environment into the surrounding large-scale structure. The latter is possible only using imaging with a sub-kiloparsec resolution and follow-up integral-field spectroscopy for a few individual cases [e.g. @ACCESSV].

The target: Shapley supercluster {#SSC}
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The ‘remote cloud of galaxies in Centaurus’ first identified by @S30 is one of the richest superclusters in the nearby Universe, consisting of as many as 25 Abell clusters [@ZZS93] in the redshift range 0.033$< z <$0.060 [@QRM95; @QMP97]. The first spectroscopic study confirming the existence of the ‘Centaurus supercluster’ was carried out by @MM87, then it was re-discovered by @SBC89 [their ‘$\alpha$-region’] as a cluster overdensity in the @ACO89 [ACO] cluster catalogue and identified by @R89 [his ‘Shapley concentration’] as an excess in galaxy number counts in the UK Schmidt Telescope Sky Survey plates.

The Shapley supercluster (hereafter SSC) because of its peculiar richness and location, lying in the direction of 