  Using the most recent results about white dwarfs in 10 open clusters, we
revisit semi-empirical estimates of the initial-final mass relation in star
clusters, with emphasis on the use of stellar evolution models. We discuss the
influence of these models on each step of the derivation. One intention of our
work is to use consistent sets of calculations both for the isochrones and the
white dwarf cooling tracks. The second one is to derive the range of systematic
errors arising from stellar evolution theory. This is achieved by using
different sources for the stellar models and by varying physical assumptions
and input data. We find that systematic errors, including the determination of
the cluster age, are dominating the initial mass values, while observational
uncertainties influence the final mass primarily. After having determined the
systematic errors, the initial-final mass relation allows us finally to draw
conclusions about the physics of the stellar models, in particular about
convective overshooting.
