Fig. 5
White dwarf luminosity functions for different density profiles of the stellar halo. The bottom panel shows, with circles, the residuals between our standard model, and, with triangles, those obtained when the density profile of a triaxial halo (Helmi 2004) and that of Navarro et al. (1996) are employed, Δ = 2(Nstd − Nρ) / (Nstd + Nρ), respectively.
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