used to calibrate the CAS+MG parameters against the Hubble sequence for our data. The signal-to-noise ratio (SNR) and spatial resolution of VST images will instead allow us to obtain reliable CAS+MG parameters up to m\*+6 ($r=21$mag), i.e. well into the dwarf galaxy regime (see Sect. \[optical\]). Finally, AAOmega and literature spectra of more luminous galaxies will provide spectral classification through line indices.

Galaxy global properties such as colours, stellar masses and star-formation rates will be derived. The contribution of both unobscured and obscured SFR need to be considered since dust-obscured cluster galaxies are common in merging clusters [e.g. @HSE09]. The $u$–band luminosity will provide a star-formation rate (SFR) indicator once calibrated using the multi–wavelength data already available in the Shapley supercluster core (see Sect. \[CD\]), by obtaining correlations between luminosity, dust extinction, and metallicity. The available mid-infrared data will provide a robust and independent indicator of obscured star formation (Sect. \[CD\]), and also allow us to identify AGN via their unusually red W1-W2 colours [e.g. @WISE10]. AGN will also be identified from their emission-line ratios or broad emission lines from the AAOmega spectra, or their X-ray emission in the supercluster core where XMM data are available.

The depths of our 