In the following we briefly outline how we will derive the quantities necessary for our study (see also Sect. \[survey\]).

As the main classification scheme of galaxies we will adopt the concentration, asymmetry and clumpiness parameters [@K85; @BJC00; @CBJ00; @C03], complemented by the M20 and Gini coefficients [@LPM04; @AvN03]. This parameter set (hereafter ‘CAS+MG’) has proven to robustly link the internal light distribution of galaxies to their formation and evolution [e.g. @SCL07; @MGZ09; @KPO14; @HMC14; @LJC08; @LJC11 and references therein]. Besides being effective in separating the different morphological types and tracing star formation, the CAS+MG scheme is particularly sensitive to their recent interaction or merging activities, making it the ideal tool to obtain a census of galaxies whose structure appears disturbed by the environment, which is crucial for our project. For a selected sample of ‘normal’ galaxies (as determined through the CAS+MG parameters) it will be possible to quantify the relevance of (pseudo-)bulges and bars as a function of the environment by surface photometry fitting.

In Fig. \[gals\] we show examples of SSC galaxies in the magnitude range from m\*-1 to m\*+4 ($r=14-19$mag). For galaxies in this magnitude range we plan to perform classical (visual) morphological classification, that will be 