Mass lost after the MS versus during the MS for models at solar metallicity (large markers) and LMC metallicity (small markers). The data are fitted with a n = 5 polynomial fit, which agrees with the data within 21.2% (root mean square relative deviation). Visually, this illustrates that the mass loss experienced during the MS of massive star evolution is a reasonable predictor of the mass loss that will be experienced in the later stages of evolution, regardless of metallicity or MS mass-loss prescription. In particular, the shape of this curve illustrates the “YSG bump” for stars that lose around 10 M_⊙ during the MS, which spend the most time in the YSG phase out of all of the models.