We present an overview of a multi-wavelength survey of the Shapley supercluster ( SSC ; z \sim 0.05 ) covering a contiguous area of 260 h ^ { -2 } _ { 70 } Mpc ^ { 2 } including the supercluster core .
The project main aim is to quantify the influence of cluster-scale mass assembly on galaxy evolution in one of the most massive structures in the local Universe .
The Shapley supercluster survey ( ShaSS ) includes nine Abell clusters ( A 3552 , A 3554 , A 3556 , A 3558 , A 3559 , A 3560 , A 3562 , AS 0724 , AS 0726 ) and two poor clusters ( SC 1327- 312 , SC 1329-313 ) showing evidence of cluster-cluster interactions .
Optical ( ugri ) and near-infrared ( K ) imaging acquired with VST and VISTA allow us to study the galaxy population down to m ^ { \star } +6 at the supercluster redshift .
A dedicated spectroscopic survey with AAOmega on the Anglo-Australian Telescope provides a magnitude-limited sample of supercluster members with 80 % completeness at \sim m ^ { \star } +3 .

We derive the galaxy density across the whole area , demonstrating that all structures within this area are embedded in a single network of clusters , groups and filaments .
The stellar mass density in the core of the SSC is always higher than 9 { \times } 10 ^ { 9 } { M } _ { \odot } { Mpc } ^ { -3 } , which is { \sim } 40 { \times } the cosmic stellar mass density for galaxies in the local Universe .
We find a new filamentary structure ( \sim 7 Mpc long in projection ) connecting the SSC core to the cluster A 3559 , as well as previously unidentified density peaks .
We perform a weak-lensing analysis of the central 1 deg ^ { 2 } field of the survey obtaining for the central cluster A 3558 a mass of M _ { 500 } = 7.63 _ { -3.40 } ^ { +3.88 } \times 10 ^ { 14 } M _ { \odot } , in agreement with X-ray based estimates .