Context : This paper is based on the multi-band VST Early-type GAlaxy Survey ( VEGAS ) with the VLT Survey Telescope ( VST ) .
We present new deep photometry of the IC 1459 group in g and r band .

Aims : The main goal of this work is to investigate the photometric properties of the IC 1459 group , and to compare our results with those obtained for other galaxy groups studied in VEGAS , in order to provide a first view of the variation of their properties as a function of the evolution of the system .

Methods : For all galaxies in the IC 1459 group , we fit isophotes and extract the azimuthally-averaged surface-brightness profiles , the position angle and ellipticity profiles as a function of the semi-major axis , as well as the average colour profile .
In each band , we estimate the total magnitudes , effective radii , mean colour , and total stellar mass for each galaxies in the group .
Then we look at the structure of the brightest galaxies and faint features in their outskirts , considering also the intragroup component .

Results : The wide field of view , long integration time , high angular resolution , and arcsec-level seeing of OmegaCAM @ VST allow us to map the light distribution of IC 1459 down to a surface brightness level of 29.26 mag arcsec ^ { -2 } in g band and 28.85 mag arcsec ^ { -2 } in r band , and out to 7 - 10 R _ { e } , and to detect the optical counterpart of HI gas around IC 1459 .
We also explore in depth three low density environments and provide information to understand how galaxies and groups properties change with the group evolution stage .

Conclusions : There is a good agreement of our results with predictions of numerical simulations regarding the structural properties of the brightest galaxies of the groups .
We suggest that the structure of the outer envelope of the BCGs ( i.e .
the signatures of past mergers and tidal interactions ) , the intra-group light and the HI amount and distribution may be used as indicators of the different evolutionary stage and mass assembly in galaxy groups .