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Using the most recent results about white dwarfs in 10 open clusters, werevisit semi-empirical estimates of the initial-final mass relation in starclusters, with emphasis on the use of stellar evolution models. We discuss theinfluence of these models on each step of the derivation. One intention of ourwork is to use consistent sets of calculations both for the isochrones and thewhite dwarf cooling tracks. The second one is to derive the range of systematicerrors arising from stellar evolution theory. This is achieved by usingdifferent sources for the stellar models and by varying physical assumptionsand input data. We find that systematic errors, including the determination ofthe cluster age, are dominating the initial mass values, while observationaluncertainties influence the final mass primarily. After having determined thesystematic errors, the initial-final mass relation allows us finally to drawconclusions about the physics of the stellar models, in particular aboutconvective overshooting.

Semi-empirical white dwarf initial-final mass relationships: a thorough analysis of systematic uncertainties due to stellar evolution models