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Studies suggest that the pollution of white dwarf (WD) atmospheres arisesfrom the accretion of minor planets, but the exact properties of pollutingmaterial, and in particular the evidence for water in some cases are not yetunderstood. Previous works studied the water retention in minor planets aroundmain-sequence and evolving host stars, in order to evaluate the possibilitythat water survives inside minor planets around WDs. However, all of thesestudies focused on small, comet-sized to moonlet-sized minor planets, when theinferred mass inside the convection zones of He-dominated WDs could actuallyalso be compatible with much more massive minor planets. In this study wetherefore explore for the first time, the water retention inside exo-planetarydwarf planets, or moderate-sized moons, with radii of the order of hundreds ofkilometres. We now cover nearly the entire potential mass range of minorplanets. The rest of the parameter space considered in this study is identicalto that of our previous study, and also includes multiple WD progenitor starmasses. We find that water retention in more massive minor planets is stillaffected by the mass of the WD progenitor, however not as much as when smallminor planets were considered. We also find that water retention is now almostalways greater than zero. On average, the detected water fraction inHe-dominated WD atmospheres should be at least 5\%, irrespective of the assumedinitial water composition, if it came from a single accretion event of an icydwarf planet or moon. This finding also strengthens the possibility of WDhabitability. To finalize our previous and current findings, we provide a codewhich may be freely used as a service to the community. The code calculates iceand water retention by interpolation, spanning the full mass range of bothminor planets and their host stars.

Post-main-sequence evolution of icy minor planets. III. water retention in dwarf planets and exo-moons and implications for white dwarf pollution