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tokens: in green, candidate members in light grey, members in red, and members with measured radial velocity in black. Figure 4. Differences between structural parameters obtained from Sérsic fits and isophotal ones. (a) Difference between r e calculated by Calderón et al. ( 2015 ) fitting a Sérsic model and the ‘isophotal’ ∼27 mag arcsec −2 ones, versus absolute and apparent T 1 magnitudes (top and bottom axes), respectively. (b) Same as plot (a) but for the difference in effective surface brightness. It is important to remark that for the two brightest galaxies ( mag), the effective radius results underestimated when using a single component profile (for NGC 3268 the difference is even larger than 1 kpc). A similar (although milder) tendency is present for S0s and cEs. It can be seen that, as expected, the confirmed dEs show mostly positive differences, while the new galaxies (mainly candidates) are the ones showing more negative differences. This effect is less noticeable if we consider a similar difference but for the effective surface brightness (Fig. 4b ). In this case, the confirmed dEs are evenly distributed about zero. 6.2 Geometrical parameters at different galactocentric radii In this section, we analyse the geometrical parameters obtained from the ellipse output for the whole sample, considering the four radial ranges (regions 1 to 4) defined in Section 4 . Fig. 5 shows the distribution of the intensity-weighted average ellipticity 〈ε〉 for the four regions, with a cross-hatched (red) histogram for faint galaxies (dEs and dSph) and an open one for the whole sample. We note that the morphological classification was done by visual inspection of each galaxy, following the criteria used in FS90. That is why we do not establish a magnitude limit (usually set around M B = −18 mag); an overlap in luminosity between bright and dwarf ellipticals can thus be seen. Figure 5. Histograms of the mean weighted ellipticity distributions, cross-hatched in red for dE and dSph and open for the whole sample. Number of galaxies in each region is indicated in parentheses. The histograms of mean ellipticity show flatter (although slightly less extended) distributions, as compared to those obtained by Chaware et al. ( 2014 ) and Hao et al. ( 2006 ), where a main peak at 〈ε〉 ∼0.1 → 0.16 is evident in regions 1 to 4, implying a dominant fraction of nearly round galaxies. Besides a similar low 〈ε〉 peak, a second peak at 〈ε〉 ≈0.3 is also evident in region 1 of our sample. This reflects the fact that most of the brighter galaxies in Antlia are lenticulars (S0), while dwarfs also tend to exhibit relatively large flattenings, despite most of them being classified as dE (dS0s are found only among the brighter dwarfs.). Figs 6 and 7 show the distributions of the weighted mean values of the Fourier coefficients 〈 a 3 / a 〉 and 〈 a 4 / a 〉. As usual, they are reasonably fitted with a single Gaussian centred at zero, except in the outermost region, where the