Fig. 4
White dwarf luminosity functions when different IMFs are considered for the stellar spheroid. The bottom panel shows, with circles, the residuals between our standard model and, with triangles, those obtained when the Salpeter (1955) and the top-heavy IMF of Suda et al. (2013) are used, Δ = 2(Nstd − NIMF) / (Nstd + NIMF), respectively.
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