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Blue compact dwarf galaxies (BCDs) form stars at, for their sizes,extraordinarily high rates. In this paper, we study what triggers thisstarburst and what is the fate of the galaxy once its gas fuel is exhausted. Weselect four BCDs with smooth outer regions, indicating them as possibleprogenitors of dwarf elliptical galaxies. We have obtained photometric andspectroscopic data with the FORS and ISAAC instruments on the VLT. We analysetheir infra-red spectra using a full spectrum fitting technique which yieldsthe kinematics of their stars and ionized gas together with their stellarpopulation characteristics. We find that the_stellar_ velocity to velocitydispersion ratio (v/sigma) of our BCDs is of the order of 1.5, similar to thatof dwarf elliptical galaxies. Thus, those objects do not require significant(if any) loss of angular momentum to fade into early type dwarfs. This findingis in discordance with previous studies, which however compared the stellarkinematics of dwarf elliptical galaxies with the gaseous kinematics of starforming dwarfs. The stellar velocity fields of our objects are very disturbedand the star-formation regions are often kinematically decoupled from the restof the galaxy. These regions can be more or less metal rich with respect to thegalactic body, and sometimes they are long lived. These characteristics preventus from pinpointing a unique trigger of the star formation, even within thesame galaxy. Gas impacts, mergers, and in-spiraling gas clumps are all possiblestar-formation ignitors for our targets.

On the origin of bursts in blue compact dwarf galaxies: clues from kinematics and stellar populations