Context : Understanding how each early-type galaxy forms and evolves is one of the objectives of the extragalactic astrophysics and cosmology .
The spatial distribution of the stellar populations inside a spheroidal system and their kinematical properties supply important informations about the formation process .
Specifically , the reconstruction of the star formation history is crucial in this context .

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 .