Fig. 5
White dwarf luminosity as a function of age for WDs which have progenitor stars with five different metallicities, for two different masses. Interpolation was used on cooling tracks calculated by several authors: Salaris et al. (2010) for Z = 0.02, Renedo et al. (2010) for Z = 0.01, Romero et al. (2015) for Z = 0.004 and Z = 0.001, and Althaus et al. (2015) for Z = 0.0001.
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