Fig. 4
Dartmouth (Dotter et al. 2008) stellar evolution tracks for stellar metallicities of 0.05 (solid lines) and 0.15 (dashed lines). The posterior distribution 1σ, 2σ and 3σ contours for a pure geometric fit of LRa06 is shown in blue. Including the stellar models in the fit allows to better constrain the density by reducing the posterior distribution to the red area.
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