SIMBAD references

We compare the mass distribution of central stars of planetary nebulae (CSPNe) with those of their progeny, white dwarfs (WD). We use a dynamical method to measure masses with an uncertainty of 0.02M_☉. The CSPN mass distribution is sharply peaked at 0.61M_☉. The WD distribution peaks at lower masses (0.58M_☉) and shows a much broader range of masses. Some of the difference can be explained if the early post-AGB evolution is faster than predicted by the Bloecker tracks. Between 30 and 50 per cent of WD may avoid the PN phase because they have too low a mass. However, the discrepancy cannot be fully resolved and WD mass distributions may have been broadened by observational or model uncertainties.