  Context: The spatial distribution of the stellar populations inside a
spheroidal system and their kinematical properties supply important
informations about the formation process. Aims: We have performed a detailed
stellar population analysis using long slit spectroscopic observations up to
almost one effective radius of two different early-type galaxies of low density
regions of the local Universe: NGC 1052, a E4 Liner prototype of a loose group
that has a stellar rotating disc, and NGC 7796, a E1 of the field which shows a
kinematically distinct core. The mean luminosity-weighted stellar age,
metallicity, and alpha/Fe ratio along both photometric axes of them have been
obtained in order to reconstruct the star formation history in their
kinematically distinct subsystems. Methods: We have measured Lick indices and
computed their radial gradients. They were compared with the predicted ones of
simple stellar population models. We have also applied a stellar population
synthesis. Results: The star characteristics are associated with their
kinematics: they are older and alpha-enhanced in the bulge of NGC 1052 and core
of NGC 7796, while they show a strong spread of alpha/Fe and age along the disc
of NGC 1052 and an outwards radial decreasing of them outside the core of NGC
7796. The age variation is possibly connected to the alpha/Fe one. Conclusions:
Both galaxies were formed by processes in which the star formation occurred
firstly at the bulge (NGC 1052) and nucleus (NGC 7796) 12-15 Gyr ago on short
timescales (0.1-1 Gyr) providing an efficient chemical enrichment by SN-II. In
the disc of NGC 1052, there is some spread of age and formation timescales
around its stars. In NGC 7796, the star formation timescale had some outwards
radial increasing along both axes.
