  We present a statistical isophotal analysis of 138 early-type galaxies in the
Antlia cluster, located at a distance of ${\sim} 35$ Mpc. The observational
material consists of CCD images of four $36$ arcmin ${\times} 36$ arcmin fields
obtained with the MOSAIC II camera at the Blanco 4-m telescope at CTIO. Our
present work supersedes previous Antlia studies in the sense that the covered
area is four times larger, the limiting magnitude is $M_{B} {\sim} -9.6$ mag,
and the surface photometry parameters of each galaxy are derived from S\'ersic
model fits extrapolated to infinity. In a companion previous study we focused
on the scaling relations obtained by means of surface photometry, and now we
present the data, on which the previous paper is based, the parameters of the
isophotal fits as well as an isophotal analysis. For each galaxy, we derive
isophotal shape parameters along the semi-major axis and search for
correlations within different radial bins. Through extensive statistical tests,
we also analyse the behaviour of these values against photometric and global
parameters of the galaxies themselves. While some galaxies do display radial
gradients in their ellipticity (${\epsilon}$) and/or their Fourier
coefficients, differences in mean values between adjacent regions are not
statistically significant. Regarding Fourier coefficients, dwarf galaxies
usually display gradients between all adjacent regions, while non-dwarfs tend
to show this behaviour just between the two outermost regions. Globally, there
is no obvious correlation between Fourier coefficients and luminosity for the
whole magnitude range ($-12 {\gtrsim} M_{V} {\gtrsim} -22$); however, dwarfs
display much higher dispersions at all radii.
