Galactic archaeology of a thick disc: Excavating ESO 533-4 with VIMOS

The formation mechanisms of thick discs are under discussion. Thick discs might have formed either at high redshift on a short time-scale or might have been built slowly over time. They may have an internal or an external origin. Here we study in detail the kinematics and the stellar populations of the thick disc of ESO533-4. ESO533-4 is a nearby bulgeless galaxy. We present the first ever IFU study of an edge-on galaxy with enough depth to study the thick disc. We exposed ESO533-4 with VIMOS@VLT for 6.5hours. The FOV covered an axial extent 0.1-0.7r_25 (1-7kpc). We used pPXF and the MILES library to obtain velocity and stellar population maps. We compared our kinematic data with simple GADGET-2 models. The apparent rotational lag of the thick disc of ESO533-4 is compatible with that expected from the combinations of two effects: differential asymmetric drift and the projection effects arising from studying a disc a few degrees (2-3) away from edge-on. Thus, ESO533-4 contains little or no retrograde material. This is compatible with three formation scenarii: the secular heating of an initially thin disc, the formation of the thick disc at high redshift in a turbulent disc phase, and its creation in a major merger event. If happening in all galaxies, this last mechanism would cause retrograde thick discs in half of them. Retrograde discs have not been observed in the five massive disc galaxies (v_c>120km s^-1) for which thick disc kinematics are known. The populations of the thin and the thick discs are separated in the Age-log(Z/Z_Sun) plane. Thus, the thin and thick discs are made of two distinct stellar populations. Although the stellar population results are not conclusive due to the high dust extinction in ESO533-4, they do not favour a secular evolution origin for the thick disc. Hence, we suggest that the thick disc of ESO533-4 formed in a relatively short event (Abridged).