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The Initial-Final Mass-Relation (IFMR) maps the masses of main sequence starsto their white dwarf descendants. The most common approach to measure the IFMRhas been to use white dwarfs in clusters. However, it has been shown that widedouble white dwarfs can also be used to measure the IFMR using a Bayesianapproach. We have observed a large sample of 90 Gaia double white dwarfs usingFORS2 on the VLT. Considering 52 DA+DA, DA+DC, and DC+DC pairs, we applied ourextended Bayesian framework to probe the IFMR in exquisite detail. Ourmonotonic IFMR is well constrained by our observations for initial masses of1-5 Msun, with the range 1-4 Msun mostly constrained to a precision of 0.03Msun or better. We add an important extension to the framework, using aBayesian mixture-model to determine the IFMR robustly in the presence ofsystems departing from single star evolution. We find a large but uncertainoutlier fraction of 59$\pm$21 percent, with outlier systems requiring anadditional $0.70^{+0.40}_{-0.22}$ Gyr uncertainty in their cooling agedifferences. However, we find that this fraction is dominated by a few systemswith massive components near 0.9 Msun, where we are most sensitive to outliers,but are also able to establish four systems as merger candidates

Measuring the Initial-Final Mass-Relation using wide double white dwarf binaries from Gaia DR3