Deep observations of the dwarf elliptical ( dE ) galaxy NGC 1396 ( M _ { V } = -16.60 , Mass \sim 4 \times 10 ^ { 8 } M _ { \odot } ) , located in the Fornax cluster , have been performed with the VLT/ MUSE spectrograph in the wavelength region from 4750 - 9350 Å .
In this paper we present a stellar population analysis studying chemical abundances , the star formation history ( SFH ) and the stellar initial mass function ( IMF ) as a function of galacto-centric distance .
Different , independent ways to analyse the stellar populations result in a luminosity-weighted age of \sim 6 Gyr and a metallicity [ Fe/H ] \sim -0.4 , similar to other dEs of similar mass .
We find unusually overabundant values of [ Ca/Fe ] \sim + 0.1 , and under-abundant Sodium , with [ Na/Fe ] values around -0.1 , while [ Mg/Fe ] is overabundant at all radii , increasing from \sim + 0.1 in the centre to \sim + 0.2 dex .
We notice a significant metallicity and age gradient within this dwarf galaxy .

To constrain the stellar IMF of NGC 1396 , we find that the IMF of NGC 1396 is consistent with either a Kroupa-like or a top-heavy distribution , while a bottom-heavy IMF is firmly ruled out .

An analysis of the abundance ratios , and a comparison with galaxies in the Local Group , shows that the chemical enrichment history of NGC 1396 is similar to the Galactic disc , with an extended star formation history .
This would be the case if the galaxy originated from a LMC-sized dwarf galaxy progenitor , which would lose its gas while falling into the Fornax cluster .