Initial-to-final mass relation of stars. The points are from the models by Miller Bertolami (2016), and the lines in the corresponding colors are the fit relations to those data points. The thick lines are at the same metallicities as the ones from the original models (Z = 0.0001, 0.001, 0.01, and 0.02) and the thin lines are at Z = 0.00001, 0.0003, 0.003, 0.014, 0.05, where the middle three values are the logarithmic midpoints of the original metallicities. Additionally, four observationally based IFMRs from nearby WD measurements at solar metallicity are shown from Cummings et al. (2018), El-Badry et al. (2018), Cunningham et al. (2024), and Hollands et al. (2024), as well as the 1σ uncertainty band of Cunningham et al. (2024).