Context : The merging of galaxies is one key aspect in our favourite hierarchical \Lambda CDM Universe and is an important channel leading to massive quiescent elliptical galaxies .
Understanding this complex transformational process is ongoing .

Aims : We aim to study NGC 7252 , which is one of the nearest major-merger galaxy remnants , observed \sim 1 Gyr after the collision of presumably two gas-rich disc galaxies .
It is therefore an ideal laboratory to study the processes inherent to the transformation of disc galaxies to ellipticals .

Methods : We obtained wide-field IFU spectroscopy with the VLT-VIMOS integral-field spectrograph covering the central 50 \arcsec \times 50 \arcsec of NGC 7252 to map the stellar and ionised gas kinematics , and the distribution and conditions of the ionised gas , revealing the extent of ongoing star formation and recent star formation history .

Results : Contrary to previous studies , we find the inner gas disc not to be counter-rotating with respect to the stars .
In addition , the stellar kinematics appear complex with a clear indication of a prolate-like rotation component which suggests a polar merger configuration .
The ongoing star formation rate is 2.2 \pm 0.6 M _ { \odot } \mathrm { yr } ^ { -1 } and implies a typical depletion time of \sim 2 Gyr given the molecular gas content .
Furthermore , the spatially resolved star formation history suggests a slight radial dependence , moving outwards at later times .
We confirm a large AGN-ionised gas cloud previously discovered \sim 5 kpc south of the nucleus , and find a higher ionisation state of the ionised gas at the galaxy centre relative to the surrounding gas disc .
Although the higher ionisation towards the centre is potentially degenerate within the central star forming ring , it may be associated with a low-luminosity AGN .

Conclusions : Although NGC 7252 has been classified as post-starburst galaxy at the centre , the elliptical-like major-merger remnant still appears very active .
A central kpc-scale gas disc has presumably re-formed quickly within the last 100 Myr after final coalescence .
The disc features ongoing star formation , implying Gyr long timescale to reach the red sequence through gas consumption alone .
While NGC 7252 is useful to probe the transformation from discs to ellipticals , it is not well-suited to study the transformation from blue to red at this point .