We present H \alpha + [ N ii ] narrow-band imaging of FCC046 and FCC207 , two dwarf ellipticals ( dES ) in the Fornax Cluster .
B-R and B-I color-maps clearly show signs of dust-absorption in FCC207 .
FCC046 has a very bright blue nucleus , offset by about 1.1 ^ { \prime \prime } with respect to the outer isophotes .
FCC046 was classified as a non-nucleated dE4 so the presence of its nucleus came as a surprise .
Moreover , FCC046 shows a pronounced lopsided shape .
Given that FCC046 is an isolated galaxy , it is unlikely that an encounter caused this asymmetry .
The emitting regions differ considerably between the two galaxies .
Whereas FCC207 has only one central emission region , FCC046 also contains fainter emission regions .
Based on broad-band colours , its disturbed shape and its very bright nucleus , FCC046 is akin to the class of amorphous dwarfs .
The central emission regions of both galaxies are barely resolved under seeing conditions of FWHM \approx 0.8 ^ { \prime \prime } and we estimate their diameters at about 60 pc .
Their H \alpha luminosities can be explained as photo-ionisation by post-AGB stars in an old population .
Some of the fainter extended emission regions in FCC046 are resolved and have diameters of the order of 50 - 150 pc and H \alpha luminosities of the order of 10 ^ { 30 } W , comparable to supernova remnants or nebulae around Wolf-Rayet stars .
Hence , FCC046 is clearly undergoing star-formation while for FCC207 the case is not as clearcut .
We estimate the mass of the H ii gas in FCC046 at M _ { H { \sc ii } } = 40 - 150 M _ { \odot } ( for T = 10 ^ { 4 } K , N _ { e } = 1000 cm ^ { -3 } ) .
The ionised-gas content of FCC207 is somewhat higher : M _ { H { \sc ii } } = 60 - 190 M _ { \odot } .