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The process of growing galactic discs 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 will be able to learn how much material, when, and how might have fallen onto the progenitor galaxy. Using publicly available data of the SDSS MaNGA DR17 survey we identified a sample of 56 counter-rotating galaxies in the MaNGA IFU survey and initiated a follow-up observational campaign at 6-m BTA telescope 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.