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We study the star-formation history of the Galactic bulge, as derived fromthe age distribution of the central stars of planetary nebulae that belong tothis stellar population. The high resolution imaging and spectroscopicobservations of 31 compact planetary nebulae are used to derive their centralstar masses. The Bloecker tracks with the cluster IFMR result in ages, whichare unexpectedly young. We find that the Bloecker post-AGB tracks need to beaccelerated by a factor of three to fit the local white dwarf masses. Thisacceleration extends the age distribution. We adjust the IFMR as a freeparameter to map the central star ages on the full age range of bulge stellarpopulations. This fit requires a steeper IFMR than the cluster relation. Wefind a star-formation rate in the Galactic bulge, which is approximatelyconstant between 3 and 10 Gyr ago. The result indicates that planetary nebulaeare mainly associated with the younger and more metal-rich bulge populations.The constant rate of star-formation between 3 and 10 Gyr agrees withsuggestions that the metal-rich component of the bulge is formed during anextended process, such as a bar interaction.

Accelerated post-AGB evolution, initial-final mass relations, and the star-formation history of the Galactic bulge