Top left panel: histogram of all the WDs formed as a function of M_ini (between 0.3 and 1 M_⊙) and Y_ini at 13 Gyr in a model that reproduces the Na distribution in NGC 6752 within the FRMS framework discussed in Paper III. Top right panel: histogram of the final masses of all the WDs at 13 Gyr. Bottom left panel: WDs present on the WD cooling curve for less than 2 Gyr (upper part of the WD cooling curve). Bottom right panel: WDs cooling for less than 500 Myr after the end of the core He burning (brighter part of the WD cooling curve).