NGC 5128 ( Centaurus A ) is one of the best example to study AGN-feedback in the local Universe .
At 13.5 kpc from the galaxy , optical filaments with recent star formation are lying along the radio-jet direction .
We used the Atacama Pathfinder EXperiment ( APEX ) to map the CO ( 2-1 ) emission all along the filaments structure .
Molecular gas mass of ( 8.2 \pm 0.5 ) \times 10 ^ { 7 } \ > M _ { \odot } was found over the 4.2 kpc-structure which represents about 3 % of the total gas mass of the NGC 5128 cold gas content .
Two dusty mostly molecular structures are identified , following the optical filaments .
The region corresponds to the crossing of the radio jet with the northern H \ @ slowromancap i @ shell , coming from a past galaxy merger .
One filament is located at the border of the H \ @ slowromancap i @ shell , while the other is entirely molecular , and devoid of H \ @ slowromancap i @ gas .
The molecular mass is comparable to the H \ @ slowromancap i @ mass in the shell , suggesting a scenario where the atomic gas was shocked and transformed in molecular clouds by the radio jet .
Comparison with combined FIR Herschel and UV GALEX estimation of star formation rates in the same regions leads to depletion times of more than 10 Gyr .
The filaments are thus less efficient than discs in converting molecular gas into stars .
Kinetic energy injection triggered by shocks all along the jet/gas interface is a possible process that appears to be consistent with MUSE line ratio diagnostics derived in a smaller region of the northern filaments .
Whether the AGN is the sole origin of this energy input and what is the dominant ( mechanical vs radiative ) mode for this process is however still to be investigated .