  We use Gemini integral field unit observations to map the stellar population
properties in the inner region ($\sim680\times470$ pc$^2$) of the galaxy NGC
6868. In order to understand the physical and chemical properties of the
stellar content of this galaxy, we performed stellar population synthesis using
the starlight code with the MILES simple stellar population models. We measured
the absorption line indices Fe4383, Mg$_2$, Mg$_b$, Fe5270, Fe5335 for the
whole FoV, and used them to derive Fe3 and [MgFe]'. These indices were used to
derive [$\alpha$/Fe]. This galaxy is dominated by old metal-rich populations
(12.6 Gyr; 1.0 and 1.6 Z$_\odot$) with a negative metallicity gradient. We also
found a recent ($\sim63$ Myr) metal-rich (1.6 Z$_{\odot}$) residual star
formation in the centre of the galaxy. A dust lane with a peak extinction in
the V band of 0.65 mag is seen. No signs of ordered stellar motion are found
and the stellar kinematics is dispersion dominated. All indices show a spatial
profile varying significantly along the FoV. Mg$_2$ shows a shallow gradient,
compatible with the occurrence of mergers in the past. Mg$_b$ and Fe3 profiles
suggest different enrichment processes for these elements. We observe three
distinct regions: for $R<100$pc and $R>220$pc, Mg$_2$, Mg$_b$ anti correlate
with respect to Fe3 and [MgFe]', and for $100 \text{pc}<R<220 \text{pc}$, they
correlate, hinting at different enrichment histories. The [$\alpha$/Fe] profile
is really complex and has a central value of $\sim 0.2$ dex. We interpret this
as the result of a past merger with another galaxy with a different
[$\alpha$/Fe] history, thus explaining the [$\alpha$/Fe] maps.
