  The process of galactic disc growing is still not fully understood. In the
majority of disk galaxies the gas and stars are located in the same plane and
rotate in the same direction. However, there are kinematically peculiar
galaxies hosting two counter-rotating stellar discs. Their origin is believed
to be the result of a past event of accretion of gas followed by star
formation. By studying such galaxies we can learn how much material, when, and
how, have fallen onto the progenitor galaxy. We identified a sample of 56
counter-rotating galaxies in the MaNGA IFU survey and initiated a follow-up
observing campaign at the 6-m telescope (BTA) aiming to determine the stellar
population properties of both stellar discs. Our preliminary results suggest
the dichotomy of the sample of counter-rotating galaxies. We found that most
massive galaxies have extended counter-rotating disks, whose contribution to
luminosity is higher than in the less massive galaxies suggestive of different
evolutionary paths.
