Our multi-wavelength survey of the Shapley supercluster (z ˜ 0.05) covers a contiguous area of 260 h _70 ^-2 Mpc^2 including the supercluster core. The project's 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 ˜ m^{star} + 3.
Shapley Supercluster Survey
Mercurio A;
2016-01-01
Abstract
Our multi-wavelength survey of the Shapley supercluster (z ˜ 0.05) covers a contiguous area of 260 h _70 ^-2 Mpc^2 including the supercluster core. The project's 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 ˜ m^{star} + 3.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
