  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.
