IFMR for WDs within star clusters. Black points represent the newly characterized WDs that have been recovered to be OC members in this work, tabulated in Table 3. The orange points denote known WDs collated from the literature (see Table 2) that have also been recovered in the clustering analysis. Their masses (M_WD) and the progenitor masses (M_WD) are adopted from the sources listed in Table 2. In purple, we plot WDs that are hosted by star clusters not considered in this study (due to the adopted distance limit or spatial constraints) listed in Salaris & Bedin (2018), Cummings et al. (2018), Richer et al. (2019), Marigo et al. (2020), Canton et al. (2021), Heyl et al. (2022), and Miller et al. (2022), and central stars of planetary nebulae are from Fragkou et al. (2019, 2022). Several IFMR fits are also shown: semi-empirical fits from Marigo et al. (2020; in red) and Cummings et al. (2018; in cyan) and the theoretical fit from Choi et al. (2016; the dashed green line).