A recent spectroscopic analysis of central stars of planetary nebulae (CSPNe) claims that the sample includes five CSPNe with masses very close to the Chandrasekhar limit of white dwarfs. This claim should be verified or discarded from the available kinematical and chemical abundance information. Kinematical parameters are extracted from Galactic orbits and compared with parameters expected for populations of different ages. The chemistry of the nebulae is compared with average values for different types. The reported high masses are not supported by our investigation. The claimed high central star masses are in contradiction with all other evidence. A more consistent picture emerges if CSPN masses close to the peak of the white dwarf mass distribution are assumed.
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